7,739 results on '"Miglio A."'
Search Results
302. The red giants in NGC 6633 as seen with CoRoT, HARPS and SOPHIE
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Poretti, Ennio, Mathias, Philippe, Barban, Caroline, Baudin, Frederic, Miglio, Andrea, Montalban, Josefina, Morel, Thierry, and Mosser, Benoit
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Astrophysics - Solar and Stellar Astrophysics - Abstract
The open cluster NGC 6633 was observed with CoRoT in 2011 and simultaneous high-resolution spectroscopy was obtained with the SOPHIE and HARPS spectrographs. One of the four targets was not found to be a cluster member. For all stars we provide estimates of the seismic and spectroscopic parameters., Comment: Proc. of the workshop "Asteroseismology of stellar populations in the Milky Way" (Sesto, 22-26 July 2013), Astrophysics and Space Science Proceedings, (eds. A. Miglio, L. Girardi, P. Eggenberger, J. Montalban)
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- 2014
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303. Solar-like oscillating stars as standard clocks and rulers for Galactic studies
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Miglio, Andrea, Girardi, Leo, Rodrigues, Thaise S., Stello, Dennis, and Chaplin, William J.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
The CoRoT and Kepler space missions have detected oscillations in hundreds of Sun-like stars and thousands of field red-giant stars. This has opened the door to a new era of stellar population studies in the Milky Way. We report on the current status and future prospects of harvesting space-based photometric data for ensemble asteroseismology, and highlight some of the challenges that need to be faced to use these stars as accurate clocks and rulers for Galactic studies., Comment: Proc. of the workshop "Asteroseismology of stellar populations in the Milky Way" (Sesto, 22-26 July 2013), Astrophysics and Space Science Proceedings, (eds. A. Miglio, L. Girardi, P. Eggenberger, J. Montalban)
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- 2014
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304. Asteroseismology of Massive Stars : Some Words of Caution
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Noels, A., Godart, M., Salmon, S., Gabriel, M., Montalban, J., and Miglio, A.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Although playing a key role in the understanding of the supernova phenomenon, the evolution of massive stars still suffers from uncertainties in their structure, even during their "quiet" main sequence phase and later on during their subgiant and helium burning phases. What is the extent of the mixed central region? In the local mixing length theory (LMLT) frame, are there structural differences using Schwarzschild or Ledoux convection criterion? Where are located the convective zone boundaries? Are there intermediate convection zones during MS and post-MS phase, and what is their extent and location? We discuss these points and show how asteroseismology could bring some light on these questions., Comment: 10 pages, 5 figures, IAU Symposium 307, New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry, G. Meynet, C. Georgy, J.H. Groh & Ph. Stee, eds
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- 2014
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305. Super-Nyquist asteroseismology of solar-like oscillators with Kepler and K2 - expanding the asteroseismic cohort at the base of the red-giant branch
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Chaplin, W. J., Elsworth, Y., Davies, G. R., Campante, T. L., Handberg, R., Miglio, A., and Basu, S.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
We consider the prospects for detecting solar-like oscillations in the "super-Nyquist" regime of long-cadence (LC) Kepler photometry, i.e., above the associated Nyquist frequency of approximately 283 {\mu}Hz. Targets of interest are cool, evolved subgiants and stars lying at the base of the red-giant branch. These stars would ordinarily be studied using the short-cadence (SC) data, since the associated SC Nyquist frequency lies well above the frequencies of the detectable oscillations. However, the number of available SC target slots is quite limited. This imposes a severe restriction on the size of the ensemble available for SC asteroseismic study.We find that archival Kepler LC data from the nominal Mission may be utilized for asteroseismic studies of targets whose dominant oscillation frequencies lie as high as approximately 500 {\mu}Hz, i.e., about 1.75- times the LC Nyquist frequency. The frequency detection threshold for the shorter-duration science campaigns of the re-purposed Kepler Mission, K2, is lower. The maximum threshold will probably lie somewhere between approximately 400 and 450 {\mu}Hz. The potential to exploit the archival Kepler and K2 LC data in this manner opens the door to increasing significantly the number of subgiant and low-luminosity red-giant targets amenable to asteroseismic analysis, overcoming target limitations imposed by the small number of SC slots.We estimate that around 400 such targets are now available for study in the Kepler LC archive. That number could potentially be a lot higher for K2, since there will be a new target list for each of its campaigns., Comment: Accepted for publication in MNRAS; 11 pages, 7 figures; reference list updated
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- 2014
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306. Why should we correct reported pulsation frequencies for stellar line-of-sight Doppler velocity shifts?
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Davies, G. R., Handberg, R., Miglio, A., Campante, T. L., Chaplin, W. J., and Elsworth, Y.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
In the age of Kepler and Corot, extended observations have provided estimates of stellar pulsation frequencies that have achieved new levels of precision, regularly exceeding fractional levels of a few parts in $10^{4}$. These high levels of precision now in principle exceed the point where one can ignore the Doppler shift of pulsation frequencies caused by the motion of a star relative to the observer. We present a correction for these Doppler shifts and use previously published pulsation frequencies to demonstrate the significance of the effect. We suggest that reported pulsation frequencies should be routinely corrected for stellar line-of-sight velocity Doppler shifts, or if a line-of-sight velocity estimate is not available, the frame of reference in which the frequencies are reported should be clearly stated., Comment: 5 pages, 1 figure, accepted for publication in MNRAS Letters
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- 2014
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307. Detection of solar-like oscillations in the bright red giant stars $\gamma$ Psc and $\theta^1$ Tau from a 190-day high-precision spectroscopic multisite campaign
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Beck, P. G., Kambe, E., Hillen, M., Corsaro, E., Van Winckel, H., Moravveji, E., De Ridder, J., Bloemen, S., Saesen, S., Mathias, P., Degroote, P., Kallinger, T., Verhoelst, T., Ando, H., Carrier, F., Acke, B., Oreiro, R., Miglio, A., Eggenberger, P., Sato, B., Zwintz, K., Pápics, P. I., Marcos-Arenal, P., Fuentes, S. A. Sans, Schmid, V. S., Waelkens, C., Østensen, R., Matthews, J. M., Yoshida, M., Izumiura, H., Koyano, H., Nagayama, S., Shimizu, Y., Okada, N., Okita, K., Sakamoto, A., Yamamuro, T., and Aerts, C.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Red giants are evolved stars which exhibit solar-like oscillations. Although a multitude of stars have been observed with space telescopes, only a handful of red-giant stars were targets of spectroscopic asteroseismic observing projects. We search for solar-like oscillations in the two bright red-giant stars $\gamma$ Psc and $\theta^1$ Tau from time series of ground-based spectroscopy and determine the frequency of the excess of oscillation power $\nu_{max}$ and the mean large frequency separation $\Delta\nu$ for both stars. The radial velocities of $\gamma$ Psc and $\theta^1$ Tau were monitored for 120 and 190 days, respectively. Nearly 9000 spectra were obtained. To reach the accurate radial velocities, we used simultaneous thorium-argon and iodine-cell calibration of our optical spectra. In addition to the spectroscopy, we acquired VLTI observations of $\gamma$ Psc for an independent estimate of the radius. Also 22 days of observations of $\theta^1$ Tau with the MOST-satellite were analysed. The frequency analysis of the radial velocity data of $\gamma$ Psc revealed an excess of oscillation power around 32 $\mu$Hz and a large frequency separation of 4.1$\pm$0.1$\mu$Hz. $\theta^1$ Tau exhibits oscillation power around 90 $\mu$Hz, with a large frequency separation of 6.9$\pm$0.2$\mu$Hz. Scaling relations indicate that $\gamma$ Psc is a star of about $\sim$1 M$_\odot$ and $\sim$10 R$_\odot$. $\theta^1$ Tau appears to be a massive star of about $\sim$2.7 M$_\odot$ and $\sim$11 R$_\odot$. The radial velocities of both stars were found to be modulated on time scales much longer than the oscillation periods. While the mass of $\theta^1$ Tau is in agreement with results from dynamical parallaxes, we find a lower mass for $\gamma$ Psc than what is given in the literature. The long periodic variability agrees with the expected time scales of rotational modulation., Comment: 15 pages, 15 figures; accepted for publication in A&A
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- 2014
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308. On the proper use of the Schwarzschild and Ledoux criteria in stellar evolution computations
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Gabriel, Maurice, Noels, Arlette, Montalban, Josefina, and Miglio, Andrea
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Astrophysics - Solar and Stellar Astrophysics - Abstract
The era of detailed asteroseismic analyses opened by space missions such as CoRoT and $\textit{Kepler}$ has highlighted the need for stellar models devoid of numerical inaccuracies, in order to be able to diagnose which physical aspects are being ignored or poorly treated in standard stellar modeling. We tackle here the important problem of fixing convective zones boundaries in the frame of the local mixing length theory. First we show that the only correct way to locate a convective zone boundary is to find, at each iteration step, through interpolations or extrapolations from points $\textit{within the convective zone}$, the mass where the radiative luminosity is equal to the total one. We then discuss two misuses of the boundary condition and the way they affect stellar modeling and stellar evolution. The first one consists in applying the neutrality condition for convective instability on the $\textit{radiative}$ side of the convective boundary. The second way of misusing the boundary condition comes from the process of fixing the convective boundary through the search for a change of sign of a possibly \textit{discontinuous} function. We show that these misuses can lead to completely wrong estimates of convective core sizes with important consequences for the following evolutionary phases. We point out the advantages of using a double mesh point at each convective zone boundaries. The specific problem of a convective shell is discussed and some remarks concerning overshooting are given., Comment: 14 pages, 10 figures, to appear in A&A
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- 2014
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309. Prospects for asteroseismic inference on the envelope helium abundance in red giant stars
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Broomhall, A. -M., Miglio, A., Montalban, J., Eggenberger, P., Chaplin, W. J., Elsworth, Y., Scuflaire, R., Ventura, P., and Verner, G. A.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Regions of rapid variation in the internal structure of a star are often referred to as acoustic glitches since they create a characteristic periodic signature in the frequencies of p modes. Here we examine the localized disturbance arising from the helium second ionization zone in red giant branch and clump stars. More specifically, we determine how accurately and precisely the parameters of the ionization zone can be obtained from the oscillation frequencies of stellar models. We use models produced by three different generation codes that not only cover a wide range of stages of evolution along the red giant phase but also incorporate different initial helium abundances. We discuss the conditions under which such fits robustly and accurately determine the acoustic radius of the second ionization zone of helium. The determined radii of the ionization zones as inferred from the mode frequencies were found to be coincident with the local maximum in the first adiabatic exponent described by the models, which is associated with the outer edge of the second ionization zone of helium. Finally, we consider whether this method can be used to distinguish stars with different helium abundances. Although a definite trend in the amplitude of the signal is observed any distinction would be difficult unless the stars come from populations with vastly different helium abundances or the uncertainties associated with the fitted parameters can be reduced. However, application of our methodology could be useful for distinguishing between different populations of red giant stars in globular clusters, where distinct populations with very different helium abundances have been observed., Comment: 16 pages, 15 figures, accepted for publication in MNRAS
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- 2014
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310. Atmospheric parameters and chemical properties of red giants in the CoRoT asteroseismology fields
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Morel, T., Miglio, A., Lagarde, N., Montalban, J., Rainer, M., Poretti, E., Eggenberger, P., Hekker, S., Kallinger, T., Mosser, B., Valentini, M., Carrier, F., Hareter, M., and Mantegazza, L.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
A precise characterisation of the red giants in the seismology fields of the CoRoT satellite is a prerequisite for further in-depth seismic modelling. High-resolution FEROS and HARPS spectra were obtained as part of the ground-based follow-up campaigns for 19 targets holding great asteroseismic potential. These data are used to accurately estimate their fundamental parameters and the abundances of 16 chemical species in a self-consistent manner. Some powerful probes of mixing are investigated (the Li and CNO abundances, as well as the carbon isotopic ratio in a few cases). The information provided by the spectroscopic and seismic data is combined to provide more accurate physical parameters and abundances. The stars in our sample follow the general abundance trends as a function of the metallicity observed in stars of the Galactic disk. After an allowance is made for the chemical evolution of the interstellar medium, the observational signature of internal mixing phenomena is revealed through the detection at the stellar surface of the products of the CN cycle. A contamination by NeNa-cycled material in the most massive stars is also discussed. With the asteroseismic constraints, these data will pave the way for a detailed theoretical investigation of the physical processes responsible for the transport of chemical elements in evolved, low- and intermediate-mass stars., Comment: Accepted for publication in A&A, 25 pages, 13 colour figures (revised version after language editing)
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- 2014
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311. The K2 Mission: Characterization and Early results
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Howell, Steve B., Sobeck, Charlie, Haas, Michael, Still, Martin, Barclay, Thomas, Mullally, Fergal, Troeltzsch, John, Aigrain, Suzanne, Bryson, Stephen T., Caldwell, Doug, Chaplin, William J., Cochran, William D., Huber, Daniel, Marcy, Geoffrey W., Miglio, Andrea, Najita, Joan R., Smith, Marcie, Twicken, J. D., and Fortney, Jonathan J.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The K2 mission will make use of the Kepler spacecraft and its assets to expand upon Kepler's groundbreaking discoveries in the fields of exoplanets and astrophysics through new and exciting observations. K2 will use an innovative way of operating the spacecraft to observe target fields along the ecliptic for the next 2-3 years. Early science commissioning observations have shown an estimated photometric precision near 400 ppm in a single 30 minute observation, and a 6-hour photometric precision of 80 ppm (both at V=12). The K2 mission offers long-term, simultaneous optical observation of thousands of objects at a precision far better than is achievable from ground-based telescopes. Ecliptic fields will be observed for approximately 75-days enabling a unique exoplanet survey which fills the gaps in duration and sensitivity between the Kepler and TESS missions, and offers pre-launch exoplanet target identification for JWST transit spectroscopy. Astrophysics observations with K2 will include studies of young open clusters, bright stars, galaxies, supernovae, and asteroseismology., Comment: 25 pages, 11 figures, Accepted to PASP
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- 2014
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312. Prospects for detecting asteroseismic binaries in Kepler data
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Miglio, A., Chaplin, W. J., Farmer, R., Kolb, U., Girardi, L., Elsworth, Y., Appourchaux, T., and Handberg, R.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Asteroseismology may in principle be used to detect unresolved stellar binary systems comprised of solar-type stars and/or red giants. This novel method relies on the detection of the presence of two solar-like oscillation spectra in the frequency spectrum of a single lightcurve. Here, we make predictions of the numbers of systems that may be detectable in data already collected by the NASA Kepler Mission. Our predictions, which are based upon TRILEGAL and BiSEPS simulations of the Kepler field of view, indicate that as many as 200 or more ``asteroseismic binaries'' may be detectable in this manner. Most of these binaries should be comprised of two He-core-burning red giants. Owing largely to the limited numbers of targets with the requisite short-cadence Kepler data, we expect only a small number of detected binaries containing solar-type stars. The predicted yield of detections is sensitive to the assumed initial mass ratio distribution of the binary components and therefore represents a sensitive calibration of the much debated initial mass ratio distribution near mass ratio unity., Comment: 21 pages, 5 figures, ApJ Letters, accepted
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- 2014
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313. Limits on surface gravities of Kepler planet-candidate host stars from non-detection of solar-like oscillations
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Campante, T. L., Chaplin, W. J., Lund, M. N., Huber, D., Hekker, S., García, R. A., Corsaro, E., Handberg, R., Miglio, A., Arentoft, T., Basu, S., Bedding, T. R., Christensen-Dalsgaard, J., Davies, G. R., Elsworth, Y. P., Gilliland, R. L., Karoff, C., Kawaler, S. D., Kjeldsen, H., Lundkvist, M., Metcalfe, T. S., Aguirre, V. Silva, and Stello, D.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present a novel method for estimating lower-limit surface gravities log g of Kepler targets whose data do not allow the detection of solar-like oscillations. The method is tested using an ensemble of solar-type stars observed in the context of the Kepler Asteroseismic Science Consortium. We then proceed to estimate lower-limit log g for a cohort of Kepler solar-type planet-candidate host stars with no detected oscillations. Limits on fundamental stellar properties, as provided by this work, are likely to be useful in the characterization of the corresponding candidate planetary systems. Furthermore, an important byproduct of the current work is the confirmation that amplitudes of solar-like oscillations are suppressed in stars with increased levels of surface magnetic activity., Comment: Accepted for publication in ApJ; 35 pages, 10 figures, 5 tables
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- 2014
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314. Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets
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Marcy, Geoffrey W., Isaacson, Howard, Howard, Andrew W., Rowe, Jason F., Jenkins, Jon M., Bryson, Stephen T., Latham, David W., Howell, Steve B., Gautier III, Thomas N., Batalha, Natalie M., Rogers, Leslie A., Ciardi, David, Fischer, Debra A., Gilliland, Ronald L., Kjeldsen, Hans, Christensen-Dalsgaard, Jørgen, Huber, Daniel, Chaplin, William J., Basu, Sarbani, Buchhave, Lars A., Quinn, Samuel N., Borucki, William J., Koch, David G., Hunter, Roger, Caldwell, Douglas A., Van Cleve, Jeffrey, Kolbl, Rea, Weiss, Lauren M., Petigura, Erik, Seager, Sara, Morton, Timothy, Johnson, John Asher, Ballard, Sarah, Burke, Chris, Cochran, William D., Endl, Michael, MacQueen, Phillip, Everett, Mark E., Lissauer, Jack J., Ford, Eric B., Torres, Guillermo, Fressin, Francois, Brown, Timothy M., Steffen, Jason H., Charbonneau, David, Basri, Gibor S., Sasselov, Dimitar D., Winn, Joshua, Sanchis-Ojeda, Roberto, Christiansen, Jessie, Adams, Elisabeth, Henze, Christopher, Dupree, Andrea, Fabrycky, Daniel C., Fortney, Jonathan J., Tarter, Jill, Holman, Matthew J., Tenenbaum, Peter, Shporer, Avi, Lucas, Philip W., Welsh, William F., Orosz, Jerome A., Bedding, T. R., Campante, T. L., Davies, G. R., Elsworth, Y., Handberg, R., Hekker, S., Karoff, C., Kawaler, S. D., Lund, M. N., Lundkvist, M., Metcalfe, T. S., Miglio, A., Aguirre, V. Silva, Stello, D., White, T. R., Boss, Alan, Devore, Edna, Gould, Alan, Prsa, Andrej, Agol, Eric, Barclay, Thomas, Coughlin, Jeff, Brugamyer, Erik, Mullally, Fergal, Quintana, Elisa V., Still, Martin, hompson, Susan E., Morrison, David, Twicken, Joseph D., Désert, Jean-Michel, Carter, Josh, Crepp, Justin R., Hébrard, Guillaume, Santerne, Alexandre, Moutou, Claire, Sobeck, Charlie, Hudgins, Douglas, Haas, Michael R., Robertson, Paul, Lillo-Box, Jorge, and Barrado, David
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Astrophysics - Earth and Planetary Astrophysics - Abstract
We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities for all of the transiting planets (41 of 42 have a false-positive probability under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than 3X the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify 6 planets with densities above 5 g/cc, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than ~2 R_earth. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O)., Comment: 94 pages, 55 figures, 25 tables. Accepted by ApJS
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- 2014
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315. Chemodynamics of the Milky Way. I. The first year of APOGEE data
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Anders, F., Chiappini, C., Santiago, B. X., Rocha-Pinto, H. J., Girardi, L., da Costa, L. N., Maia, M. A. G., Steinmetz, M., Minchev, I., Schultheis, M., Boeche, C., Miglio, A., Montalbán, J., Schneider, D. P., Beers, T. C., Cunha, K., Prieto, C. Allende, Balbinot, E., Bizyaev, D., Brauer, D. E., Brinkmann, J., Frinchaboy, P. M., Pérez, A. E. García, Hayden, M. R., Hearty, F. R., Holtzman, J., Johnson, J., Kinemuchi, K., Majewski, S. R., Malanushenko, E., Malanushenko, V., Nidever, D. L., O'Connell, R. W., Pan, K., Robin, A. C., Schiavon, R. P., Shetrone, M., Skrutskie, M. F., Smith, V. V., Stassun, K., and Zasowski, G.
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Astrophysics - Galaxy Astrophysics - Abstract
We investigate the chemo-kinematic properties of the Milky Way disc by exploring the first year of data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE), and compare our results to smaller optical high-resolution samples in the literature, as well as results from lower resolution surveys such as GCS, SEGUE and RAVE. We start by selecting a high-quality sample in terms of chemistry ($\sim$ 20.000 stars) and, after computing distances and orbital parameters for this sample, we employ a number of useful subsets to formulate constraints on Galactic chemical and chemodynamical evolution processes in the Solar neighbourhood and beyond (e.g., metallicity distributions -- MDFs, [$\alpha$/Fe] vs. [Fe/H] diagrams, and abundance gradients). Our red giant sample spans distances as large as 10 kpc from the Sun. We find remarkable agreement between the recently published local (d $<$ 100 pc) high-resolution high-S/N HARPS sample and our local HQ sample (d $<$ 1 kpc). The local MDF peaks slightly below solar metallicity, and exhibits an extended tail towards [Fe/H] $= -$1, whereas a sharper cut-off is seen at larger metallicities. The APOGEE data also confirm the existence of a gap in the [$\alpha$/Fe] vs. [Fe/H] abundance diagram. When expanding our sample to cover three different Galactocentric distance bins, we find the high-[$\alpha$/Fe] stars to be rare towards the outer zones, as previously suggested in the literature. For the gradients in [Fe/H] and [$\alpha$/Fe], measured over a range of 6 $ < $ R $ <$ 11 kpc in Galactocentric distance, we find a good agreement with the gradients traced by the GCS and RAVE dwarf samples. For stars with 1.5 $<$ z $<$ 3 kpc, we find a positive metallicity gradient and a negative gradient in [$\alpha$/Fe]., Comment: 25 pages, 17 figures. A&A, in press
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- 2013
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316. Colorectal cancer screening: Assessment of CEACAM6, LGALS4, TSPAN8 and COL1A2 as blood markers in faecal immunochemical test negative subjects
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Enea Ferlizza, Rossella Solmi, Rossella Miglio, Elena Nardi, Gabriella Mattei, Michela Sgarzi, and Mattia Lauriola
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Blood mRNA ,Faecal immunochemical test ,CEACAM6 ,LGALS4 ,TSPAN8 ,COL1A2 ,Medicine (General) ,R5-920 ,Science (General) ,Q1-390 - Abstract
Prevention is essential to reduce Colorectal Cancer (CRC) mortality. We previously reported a panel of four genes: CEACAM6, LGALS4, TSPAN8, COL1A2 (CELTiC) able to discriminate patients with CRC. Here, we assessed the CELTiC panel by quantitative polymerase chain reaction, in the blood of 174 healthy subjects, who resulted negative to the faecal immunochemical test (FITN). Using non-parametric statistic and multinomial logistic models, the FITN were compared to previously analysed subjects: 36 false positive FIT (NFIT), who were negative at colonoscopy, 36 patients with low risk lesions (LR) and 92 patients with high risk lesions or CRC (HR/CRC). FITN showed a significantly lower expression of the four genes when compared to HR/CRC. Moreover, FITN showed a significantly lower expression of TSPAN8 and COL1A2 compared to NFIT and LR patients.The multinomial logistic model confirmed that TSPAN8 alone specifically discriminated FITN from NFIT, LR and HR/CRC, while LGALS4 was able to differentiate FITN from false positive FIT. Finally, ROC curves analysis of the comparisons between FITN and HR/CRC, LR or NFIT reported AUC greater than 0.87, with a sensitivity and specificity of 83% and 76%, respectively. The CELTiC panel was confirmed a useful tool to identify CRC patients and to discriminate false FIT positive subjects.
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- 2020
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317. Histologic subtyping affecting outcome of triple negative breast cancer: a large Sardinian population-based analysis
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Francesca Sanges, Matteo Floris, Paolo Cossu-Rocca, Maria R. Muroni, Giovanna Pira, Silvana Anna Maria Urru, Renata Barrocu, Silvano Gallus, Cristina Bosetti, Maurizio D’Incalci, Alessandra Manca, Maria Gabriela Uras, Ricardo Medda, Elisabetta Sollai, Alma Murgia, Dolores Palmas, Francesco Atzori, Angelo Zinellu, Francesca Cambosu, Tiziana Moi, Massimo Ghiani, Vincenzo Marras, Maria Cristina Santona, Luisa Canu, Enrichetta Valle, Maria Giuseppina Sarobba, Daniela Onnis, Anna Asunis, Sergio Cossu, Sandra Orrù, and Maria Rosaria De Miglio
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Triple negative breast cancer ,Clinico-pathological features ,Prognosis ,Histologic special type ,Tumor size ,Metastatic lymph node ,Neoplasms. Tumors. Oncology. Including cancer and carcinogens ,RC254-282 - Abstract
Abstract Background Triple Negative breast cancer (TNBC) includes a heterogeneous group of tumors with different clinico-pathological features, molecular alterations and treatment responsivity. Our aim was to evaluate the clinico-pathological heterogeneity and prognostic significance of TNBC histologic variants, comparing “special types” to high-grade invasive breast carcinomas of no special type (IBC-NST). Methods This study was performed on data obtained from TNBC Database, including pathological features and clinical records of 1009 TNBCs patients diagnosed between 1994 and 2015 in the four most important Oncology Units located in different hospitals in Sardinia, Italy. Kaplan-Meier analysis, log-rank test and multivariate Cox proportional-hazards regression were applied for overall survival (OS) and disease free survival (DFS) according to TNBC histologic types. Results TNBC “special types” showed significant differences for several clinico-pathological features when compared to IBC-NST. We observed that in apocrine carcinomas as tumor size increased, the number of metastatic lymph nodes manifestly increased. Adenoid cystic carcinoma showed the smallest tumor size relative to IBC-NST. At five-year follow-up, OS was 92.1, 100.0, and 94.5% for patients with apocrine, adenoid cystic and medullary carcinoma, respectively; patients with lobular and metaplastic carcinoma showed the worst OS, with 79.7 and 84.3%, respectively. At ten-years, patients with adenoid cystic (100.0%) and medullary (94.5%) carcinoma showed a favourable prognosis, whereas patients with lobular carcinoma showed the worst prognosis (73.8%). TNBC medullary type was an independent prognostic factor for DFS compared to IBC-NST. Conclusions Our study confirms that an accurate and reliable histopathologic definition of TNBC subtypes has a significant clinical utility and is effective in the therapeutic decision-making process, with the aim to develop innovative and personalized treatments.
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- 2020
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318. MTHFR, XRCC1 and OGG1 genetic polymorphisms in breast cancer: a case-control study in a population from North Sardinia
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Matteo Floris, Daria Sanna, Paolo Castiglia, Carlo Putzu, Valeria Sanna, Antonio Pazzola, Maria Rosaria De Miglio, Francesca Sanges, Giovanna Pira, Antonio Azara, Emanuele Lampis, Antonello Serra, Ciriaco Carru, Maristella Steri, Flavia Costanza, Marco Bisail, and Maria Rosaria Muroni
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Mediterranean population ,MTHFR SNPs ,XRCC1 SNPs ,OGG1 SNPs ,Neoplasms. Tumors. Oncology. Including cancer and carcinogens ,RC254-282 - Abstract
Abstract Background Despite conflicting results, considerable evidence suggests the association between single nucleotide polymorphisms in MTHFR, XRCC1 and OGG1 genes and, risk of developing breast cancer. Here a case-control study is reported, including 135 breat cancer patients and 112 healthy women, all representative of Northern Sardinian population. Methods Polymerase chain reaction/restriction fragment length polymorphism method was used to determine the genotypes of five polymorphisms: MTHFR C677T (rs1801133) and A1298C (rs1801131), XRCC1 Arg194Trp (rs1799782) and Arg399Gln (rs25487) and OGG1 Ser326Cys (rs1052133). Allelic, genotypic and haplotype association analyses with disease risk and clinicopathological parameters were performed. Results A nominally significant association with breast cancer risk was observed for MTHFR C677T polymorphism heterozygous genotype in the codominant model (OR: 0.57, 95% CI: 0.32–1.00, p = 0.049) and for Cys/Cys genotype of the OGG1 Ser326Cys polymorphism in the recessive model (OR: 0.23, 95% CI: 0.05–1.11, p = 0.0465). No significant differences were found at genotype-level for A1298C polymorphism of the MTHFR gene and Arg194Trp and Arg399Gln of the XRCC1 gene. Furthermore, the OGG1 and XRCC1 rs25487 polymorphisms were nominally associated with PgR, Her2 status and with sporadic breast cancer, respectively. Conclusions Based on genetic characteristics of individuals included in this study, results suggest that MTHFR CT and OGG1 Cys/Cys genotypes have a protective effect that may have an influence on breast cancer risk in a representative Northern Sardinian population.
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- 2020
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319. NASCITA Italian birth cohort study: a study protocol
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Claudia Pansieri, Antonio Clavenna, Chiara Pandolfini, Michele Zanetti, Maria Grazia Calati, Daniela Miglio, Massimo Cartabia, Federica Zanetto, and Maurizio Bonati
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Clinical trial protocol [publication type] ,Cohort studies ,Infant, newborn ,Child ,Infant ,Health ,Pediatrics ,RJ1-570 - Abstract
Abstract Background Young children’s healthy development depends on nurturing care, which ensures health, nutrition, responsive caregiving, safety and security, and early learning. Infancy and childhood are characterized by rapid growth and development, and these two factors contribute largely to determining health status and well-being across the lifespan. Identification of modifiable risk factors and prognostic factors during the critical periods of life will contribute to the development of effective prevention and intervention strategies. The NASCITA (NAscere e creSCere in ITAlia) study was created to evaluate physical, cognitive, and psychological development, health status and health resource utilization during the first six years of life in a cohort of newborns, and to evaluate potential associated factors. Methods NASCITA is an ongoing, dynamic, prospective, population-based birth cohort study of an expected number of more than 5000 newborns who will be recruited in 22 national geographic clusters starting in 2019. It was designed to follow children from birth to school entry age for a wide range of determinants, disorders, and diseases. Recruitment of the newborns (and their parents) will take place during the first routine well-child visit, which takes place at the office of the pediatrician assigned to them by the local health unit of residence, and which is scheduled for all newborns born in Italy within the first 45 days of their life. Data will be web-based and collected by the family pediatricians during each of the 7 standard well-child visits scheduled for all children during their first 6 years of life. Information on every contact with the enrolled children in addition to these prescheduled visits will be also recorded. Discussion The NASCITA cohort study provides a framework in which children are followed from birth to six-years of age. NASCITA will broaden our understanding of the contribution of early-life factors to infant and child health and development. NASCITA provides opportunities to initiate new studies, also experimental ones, in parts of the cohort, and will contribute relevant information on determinants and health outcomes to policy and decision makers. Cohort details can be found on https://coortenascita.marionegri.it. Trial registration Clinicaltrials.gov: NCT03894566. Ethics committee approval: 6 February 2019, Verbale N 59.
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- 2020
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320. Understanding Outsourcing and Subcontracting : An Approach from the Theory of Surplus Value
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Miglio, Martín Rodríguez and Breña, Mariana Ortega
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- 2018
321. Author Correction: In-plane selective area InSb–Al nanowire quantum networks
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Op het Veld, Roy L. M., Xu, Di, Schaller, Vanessa, Verheijen, Marcel A., Peters, Stan M. E., Jung, Jason, Tong, Chuyao, Wang, Qingzhen, de Moor, Michiel W. A., Hesselmann, Bart, Vermeulen, Kiefer, Bommer, Jouri D. S., Lee, Joon Sue, Sarikov, Andrey, Pendharkar, Mihir, Marzegalli, Anna, Koelling, Sebastian, Kouwenhoven, Leo P., Miglio, Leo, Palmstrøm, Chris J., Zhang, Hao, and Bakkers, Erik P. A. M.
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- 2021
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322. Pre-operative management of Pleomorphic and florid lobular carcinoma in situ of the breast: Report of a large multi-institutional series and review of the literature
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Foschini, Maria P., Miglio, Rossella, Fiore, Roberta, Baldovini, Chiara, Castellano, Isabella, Callagy, Grace, Bianchi, Simonetta, Kaya, Handan, Amendoeira, Isabel, Querzoli, Patrizia, Poli, Francesca, Scatena, Cristian, Cordoba, Alicia, Pietribiasi, Francesca, Kovács, Anikó, Faistova, Hana, Cserni, Gábor, and Quinn, Cecily
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- 2019
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323. Sanctions in the EMU Economic Pillar
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Costamagna, Francesco, primary and Miglio, Alberto, additional
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- 2021
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324. Introduction
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Montaldo, Stefano, primary, Costamagna, Francesco, additional, and Miglio, Alberto, additional
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- 2021
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325. Prospects for Galactic and stellar astrophysics with asteroseismology of giant stars in the TESS continuous viewing zones and beyond
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J Ted Mackereth, Andrea Miglio, Yvonne Elsworth, Benoit Mosser, Savita Mathur, Rafael A Garcia, Domenico Nardiello, Oliver J Hall, Mathieu Vrard, Warrick H Ball, Sarbani Basu, Rachael L Beaton, Paul G Beck, Maria Bergemann, Diego Bossini, Luca Casagrande, Tiago L Campante, William J Chaplin, Cristina Chiappini, Léo Girardi, Andreas Christ Sølvsten Jørgensen, Saniya Khan, Josefina Montalbán, Martin B Nielsen, Marc H Pinsonneault, Thaíse S Rodrigues, Aldo Serenelli, Victor Silva Aguirre, Dennis Stello, Jamie Tayar, Johanna Teske, Jennifer L van Saders, and Emma Willett
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- 2021
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326. Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi
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Chaplin, William J., Serenelli, Aldo M., Miglio, Andrea, Morel, Thierry, Mackereth, J. Ted, Vincenzo, Fiorenzo, Kjeldsen, Hans, Basu, Sarbani, Ball, Warrick H., Stokholm, Amalie, Verma, Kuldeep, Mosumgaard, Jakob Rørsted, Silva Aguirre, Victor, Mazumdar, Anwesh, Ranadive, Pritesh, Antia, H. M., Lebreton, Yveline, Ong, Joel, Appourchaux, Thierry, Bedding, Timothy R., Christensen-Dalsgaard, Jørgen, Creevey, Orlagh, García, Rafael A., Handberg, Rasmus, Huber, Daniel, Kawaler, Steven D., Lund, Mikkel N., Metcalfe, Travis S., Stassun, Keivan G., Bazot, Michäel, Beck, Paul G., Bell, Keaton J., Bergemann, Maria, Buzasi, Derek L., Benomar, Othman, Bossini, Diego, Bugnet, Lisa, Campante, Tiago L., Orhan, Zeynep Çelik, Corsaro, Enrico, González-Cuesta, Lucía, Davies, Guy R., Di Mauro, Maria Pia, Egeland, Ricky, Elsworth, Yvonne P., Gaulme, Patrick, Ghasemi, Hamed, Guo, Zhao, Hall, Oliver J., Hasanzadeh, Amir, Hekker, Saskia, Howe, Rachel, Jenkins, Jon M., Jiménez, Antonio, Kiefer, René, Kuszlewicz, James S., Kallinger, Thomas, Latham, David W., Lundkvist, Mia S., Mathur, Savita, Montalbán, Josefina, Mosser, Benoit, Bedón, Andres Moya, Nielsen, Martin Bo, Örtel, Sibel, Rendle, Ben M., Ricker, George R., Rodrigues, Thaíse S., Roxburgh, Ian W., Safari, Hossein, Schofield, Mathew, Seager, Sara, Smalley, Barry, Stello, Dennis, Szabó, Róbert, Tayar, Jamie, Themeßl, Nathalie, Thomas, Alexandra E. L., Vanderspek, Roland K., van Rossem, Walter E., Vrard, Mathieu, Weiss, Achim, White, Timothy R., Winn, Joshua N., and Yıldız, Mutlu
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- 2020
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327. Correction to: Prescription appropriateness of anti-diabetes drugs in elderly patients hospitalized in a clinical setting: evidence from the REPOSI Register (Internal and Emergency Medicine, (2023), 18, 4, (1049-1063), 10.1007/s11739-023-03254-3)
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Succurro E., Succurro, E, Novella, A, Nobili, A, Giofre, F, Arturi, F, Sciacqua, A, Andreozzi, F, Pietrangelo, A, Sesti, G, Perticone, F, Violi, F, Corrao, S, Marengoni, A, Tettamanti, M, Pasina, L, Franchi, C, Miglio, G, Ardoino, I, Cantiero, S, Prisco, D, Silvestri, E, Emmi, G, Bettiol, A, Mattioli, I, Mazzetti, M, Biolo, G, Zanetti, M, Bartelloni, G, Zaccari, M, Chiuch, M, Martini, I, Pirro, M, Lupattelli, G, Bianconi, V, Alcidi, R, Giotta, A, Mannarino, M, Girelli, D, Busti, F, Marchi, G, Barbagallo, M, Dominguez, L, Beneduce, V, Cacioppo, F, Natoli, G, Mularo, S, Raspanti, M, Argano, C, Cavallaro, F, Zoli, M, Orio, G, Magnolfi, E, Serafini, G, Brunori, M, Lazzari, I, Simili, A, Fabio, G, De Amicis, M, Luca, G, Scaramellini, N, Stefano, V, Leoni, S, Seghezzi, S, Di Mauro, A, Maira, D, Mancarella, M, Lucchi, T, Clerici, M, Bonini, G, Conti, F, Prolo, S, Fabrizi, M, Martelengo, M, Vigani, G, Nicolini, P, Sabatino, A, Miceli, E, Pisati, M, Pitotti, L, Antoci, V, Cambie, G, Pontremoli, R, Beccati, V, Nobili, G, Leoncini, G, Alberto, J, Cattaneo, F, Anastasio, L, Sofia, L, Carbone, M, Cipollone, F, Rossi, I, Valeriani, E, D'Ardes, D, Cipollone, A, Esposito, L, Sestili, S, Angelucci, E, Mancuso, G, Calipari, D, Bartone, M, Manetti, R, Sircana, M, Berria, M, Delitala, A, Muscaritoli, M, Molfino, A, Petrillo, E, Giorgi, A, Gracin, C, Imbimbo, G, Romanelli, G, Volpini, A, Lucente, D, Manzoni, F, Pirozzi, A, Zucchelli, A, Geneletti, T, Picardi, A, Bellelli, G, Corsi, M, Antonucci, C, Sidoli, C, Principato, G, Bonfanti, A, Szabo, H, Mazzola, P, Piazzoli, A, Tassone, B, De Falco, A, Negro, E, Brenna, M, Trotta, L, Fabris, F, Bertozzi, I, Bogoni, G, Prandini, T, Ratti, F, Zurlo, C, Cerruti, L, Cosi, E, Reni, E, Manfredini, R, Boari, B, Tiseo, R, Savrie, C, Fabbian, F, Paolisso, G, Catalano, C, Meo, I, Sabba, C, Suppressa, P, De Vincenzo, G, Comitangelo, A, Amoruso, E, Custodero, C, Re, G, Barnaba, I, Schilardi, A, Fenoglio, L, Falcetta, A, D'Aniano, S, Tiraboschi, S, Cespiati, A, Oberti, G, Sigon, G, Cinque, F, Colavolpe, L, Curra, J, Alletto, F, Benzoni, G, Peyvandi, F, Rossio, R, Colombo, G, Agosti, P, Pagliaro, E, Semproni, E, Canetta, C, Monzani, V, Savojardo, V, Ceriani, G, Folli, C, Tognin, T, Purrello, F, Pino, A, Piro, S, Rozzini, R, Falanga, L, Boffelli, S, Ferrandina, C, Mazzeo, F, Spazzini, E, Cono, G, Cesaroni, G, Perri, L, Guasti, L, Rotunno, F, Castiglioni, L, Maresca, A, Squizzato, A, Campiotti, L, Grossi, A, Dentali, F, Behnke, V, Perticone, M, Maio, R, Scozzafava, A, Condoleo, V, Clausi, E, Armentaro, G, Panza, A, Stanghellini, V, Ruggeri, E, Vecchio, S, Benzoni, I, Minisola, S, Colangelo, L, Cilli, M, Labbadia, G, Pepe, J, Castellino, P, Zanoli, L, Gaudio, A, Xourafa, A, Spichetti, C, Torre, S, Gennaro, A, Ballestrero, A, Ferrando, F, Gonella, R, Cerminara, D, Setti, P, Traversa, C, Scarsi, C, Famularo, G, Tarsitani, P, Morretti, T, Aglitti, A, Giacco, S, Firinu, D, Costanzo, G, Chessa, S, Montalto, G, Licata, A, Rizzo, A, Corica, F, Basile, G, Catalano, A, Bellone, F, Principato, C, Cocuzza, A, Mecocci, P, Ruggiero, C, Boccardi, V, Meschi, T, Ticinesi, A, Nouvenne, A, Pirisi, M, Sola, D, Bellan, M, Quadri, R, Larovere, E, Novelli, M, Simeone, E, Scurti, R, Tolloso, F, Tarquini, R, Valoriani, A, Dolenti, S, Vannini, G, Volpi, R, Bocchi, P, Vignali, A, Harari, S, Lonati, C, Napoli, F, Aiello, I, Salvatore, T, Monaco, L, Ricozzi, C, Coviello, F, Catalini, C, Pilotto, A, Indiano, I, Gandolfo, F, Gonella, D, Nuti, R, Valenti, R, Ruvio, M, Cappelli, S, Palazzuoli, A, Durante, V, Tirotta, D, Eusebi, G, Tresoldi, M, Bozzolo, E, Damanti, S, Porta, M, Gino, M, Pari, B, Pace, E, Succurro E., Novella A., Nobili A., Giofre F., Arturi F., Sciacqua A., Andreozzi F., Pietrangelo A., Sesti G., Perticone F., Violi F., Corrao S., Marengoni A., Tettamanti M., Pasina L., Franchi C., Miglio G., Ardoino I., Cantiero S., Prisco D., Silvestri E., Emmi G., Bettiol A., Mattioli I., Mazzetti M., Biolo G., Zanetti M., Bartelloni G., Zaccari M., Chiuch M., Martini I., Pirro M., Lupattelli G., Bianconi V., Alcidi R., Giotta A., Mannarino M. R., Girelli D., Busti F., Marchi G., Barbagallo M., Dominguez L., Beneduce V., Cacioppo F., Natoli G., Mularo S., Raspanti M., Argano C., Cavallaro F., Zoli M., Orio G., Magnolfi E., Serafini G., Brunori M., Lazzari I., Simili A., Fabio G., De Amicis M. M., Luca G., Scaramellini N., Stefano V., Leoni S., Seghezzi S., Di Mauro A. D., Maira D., Mancarella M., Lucchi T., Clerici M., Bonini G., Conti F., Prolo S., Fabrizi M., Martelengo M., Vigani G., Nicolini P., Sabatino A., Miceli E., Pisati M., Pitotti L., Antoci V., Cambie G., Pontremoli R., Beccati V., Nobili G., Leoncini G., Alberto J., Cattaneo F., Anastasio L., Sofia L., Carbone M., Cipollone F., Rossi I., Valeriani E., D'Ardes D., Cipollone A., Esposito L., Sestili S., Angelucci E., Mancuso G., Calipari D., Bartone M., Manetti R., Sircana M., Berria M., Delitala A., Muscaritoli M., Molfino A., Petrillo E., Giorgi A., Gracin C., Imbimbo G., Romanelli G., Volpini A., Lucente D., Manzoni F., Pirozzi A., Zucchelli A., Geneletti T., Picardi A., Bellelli G., Corsi M., Antonucci C., Sidoli C., Principato G., Bonfanti A., Szabo H., Mazzola P., Piazzoli A., Tassone B., De Falco A. B. T., Negro E., Brenna M., Trotta L., Fabris F., Bertozzi I., Bogoni G., Prandini T., Ratti F., Zurlo C., Cerruti L., Cosi E., Reni E., Manfredini R., Boari B., Tiseo R., Savrie C., Fabbian F., Paolisso G., Catalano C., Meo I., Sabba C., Suppressa P., De Vincenzo G. M., Comitangelo A., Amoruso E., Custodero C., Re G., Barnaba I., Schilardi A., Fenoglio L., Falcetta A., D'Aniano S., Tiraboschi S., Cespiati A., Oberti G., Sigon G., Cinque F., Colavolpe L., Curra J., Alletto F., Benzoni G., Peyvandi F., Rossio R., Colombo G., Agosti P., Pagliaro E., Semproni E., Canetta C., Monzani V., Savojardo V., Ceriani G., Folli C., Tognin T., Purrello F., Pino A., Piro S., Rozzini R., Falanga L., Boffelli S., Ferrandina C., Mazzeo F., Spazzini E., Cono G., Cesaroni G., Perri L., Guasti L., Rotunno F., Castiglioni L., Maresca A., Squizzato A., Campiotti L., Grossi A., Dentali F., Behnke V., Perticone M., Maio R., Scozzafava A., Condoleo V., Clausi E., Armentaro G., Panza A., Stanghellini V., Ruggeri E., Vecchio S., Benzoni I., Minisola S., Colangelo L., Cilli M., Labbadia G., Pepe J., Castellino P., Zanoli L., Gaudio A., Xourafa A., Spichetti C., Torre S., Gennaro A., Ballestrero A., Ferrando F., Gonella R., Cerminara D., Setti P., Traversa C., Scarsi C., Famularo G., Tarsitani P., Morretti T., Aglitti A., Giacco S., Firinu D., Costanzo G., Chessa S., Montalto G., Licata A., Rizzo A., Corica F., Basile G., Catalano A., Bellone F., Principato C., Cocuzza A., Mecocci P., Ruggiero C., Boccardi V., Meschi T., Ticinesi A., Nouvenne A., Pirisi M., Sola D., Bellan M., Quadri R., Larovere E., Novelli M., Simeone E., Scurti R., Tolloso F., Tarquini R., Valoriani A., Dolenti S., Vannini G., Volpi R., Bocchi P., Vignali A., Harari S., Lonati C., Napoli F., Aiello I., Salvatore T., Monaco L., Ricozzi C., Coviello F., Catalini C., Pilotto A., Indiano I., Gandolfo F., Gonella D., Nuti R., Valenti R., Ruvio M., Cappelli S., Palazzuoli A., Durante V., Tirotta D., Eusebi G., Tresoldi M., Bozzolo E., Damanti S., Porta M., Gino M., Pari B., Pace E., Succurro E., Succurro, E, Novella, A, Nobili, A, Giofre, F, Arturi, F, Sciacqua, A, Andreozzi, F, Pietrangelo, A, Sesti, G, Perticone, F, Violi, F, Corrao, S, Marengoni, A, Tettamanti, M, Pasina, L, Franchi, C, Miglio, G, Ardoino, I, Cantiero, S, Prisco, D, Silvestri, E, Emmi, G, Bettiol, A, Mattioli, I, Mazzetti, M, Biolo, G, Zanetti, M, Bartelloni, G, Zaccari, M, Chiuch, M, Martini, I, Pirro, M, Lupattelli, G, Bianconi, V, Alcidi, R, Giotta, A, Mannarino, M, Girelli, D, Busti, F, Marchi, G, Barbagallo, M, Dominguez, L, Beneduce, V, Cacioppo, F, Natoli, G, Mularo, S, Raspanti, M, Argano, C, Cavallaro, F, Zoli, M, Orio, G, Magnolfi, E, Serafini, G, Brunori, M, Lazzari, I, Simili, A, Fabio, G, De Amicis, M, Luca, G, Scaramellini, N, Stefano, V, Leoni, S, Seghezzi, S, Di Mauro, A, Maira, D, Mancarella, M, Lucchi, T, Clerici, M, Bonini, G, Conti, F, Prolo, S, Fabrizi, M, Martelengo, M, Vigani, G, Nicolini, P, Sabatino, A, Miceli, E, Pisati, M, Pitotti, L, Antoci, V, Cambie, G, Pontremoli, R, Beccati, V, Nobili, G, Leoncini, G, Alberto, J, Cattaneo, F, Anastasio, L, Sofia, L, Carbone, M, Cipollone, F, Rossi, I, Valeriani, E, D'Ardes, D, Cipollone, A, Esposito, L, Sestili, S, Angelucci, E, Mancuso, G, Calipari, D, Bartone, M, Manetti, R, Sircana, M, Berria, M, Delitala, A, Muscaritoli, M, Molfino, A, Petrillo, E, Giorgi, A, Gracin, C, Imbimbo, G, Romanelli, G, Volpini, A, Lucente, D, Manzoni, F, Pirozzi, A, Zucchelli, A, Geneletti, T, Picardi, A, Bellelli, G, Corsi, M, Antonucci, C, Sidoli, C, Principato, G, Bonfanti, A, Szabo, H, Mazzola, P, Piazzoli, A, Tassone, B, De Falco, A, Negro, E, Brenna, M, Trotta, L, Fabris, F, Bertozzi, I, Bogoni, G, Prandini, T, Ratti, F, Zurlo, C, Cerruti, L, Cosi, E, Reni, E, Manfredini, R, Boari, B, Tiseo, R, Savrie, C, Fabbian, F, Paolisso, G, Catalano, C, Meo, I, Sabba, C, Suppressa, P, De Vincenzo, G, Comitangelo, A, Amoruso, E, Custodero, C, Re, G, Barnaba, I, Schilardi, A, Fenoglio, L, Falcetta, A, D'Aniano, S, Tiraboschi, S, Cespiati, A, Oberti, G, Sigon, G, Cinque, F, Colavolpe, L, Curra, J, Alletto, F, Benzoni, G, Peyvandi, F, Rossio, R, Colombo, G, Agosti, P, Pagliaro, E, Semproni, E, Canetta, C, Monzani, V, Savojardo, V, Ceriani, G, Folli, C, Tognin, T, Purrello, F, Pino, A, Piro, S, Rozzini, R, Falanga, L, Boffelli, S, Ferrandina, C, Mazzeo, F, Spazzini, E, Cono, G, Cesaroni, G, Perri, L, Guasti, L, Rotunno, F, Castiglioni, L, Maresca, A, Squizzato, A, Campiotti, L, Grossi, A, Dentali, F, Behnke, V, Perticone, M, Maio, R, Scozzafava, A, Condoleo, V, Clausi, E, Armentaro, G, Panza, A, Stanghellini, V, Ruggeri, E, Vecchio, S, Benzoni, I, Minisola, S, Colangelo, L, Cilli, M, Labbadia, G, Pepe, J, Castellino, P, Zanoli, L, Gaudio, A, Xourafa, A, Spichetti, C, Torre, S, Gennaro, A, Ballestrero, A, Ferrando, F, Gonella, R, Cerminara, D, Setti, P, Traversa, C, Scarsi, C, Famularo, G, Tarsitani, P, Morretti, T, Aglitti, A, Giacco, S, Firinu, D, Costanzo, G, Chessa, S, Montalto, G, Licata, A, Rizzo, A, Corica, F, Basile, G, Catalano, A, Bellone, F, Principato, C, Cocuzza, A, Mecocci, P, Ruggiero, C, Boccardi, V, Meschi, T, Ticinesi, A, Nouvenne, A, Pirisi, M, Sola, D, Bellan, M, Quadri, R, Larovere, E, Novelli, M, Simeone, E, Scurti, R, Tolloso, F, Tarquini, R, Valoriani, A, Dolenti, S, Vannini, G, Volpi, R, Bocchi, P, Vignali, A, Harari, S, Lonati, C, Napoli, F, Aiello, I, Salvatore, T, Monaco, L, Ricozzi, C, Coviello, F, Catalini, C, Pilotto, A, Indiano, I, Gandolfo, F, Gonella, D, Nuti, R, Valenti, R, Ruvio, M, Cappelli, S, Palazzuoli, A, Durante, V, Tirotta, D, Eusebi, G, Tresoldi, M, Bozzolo, E, Damanti, S, Porta, M, Gino, M, Pari, B, Pace, E, Succurro E., Novella A., Nobili A., Giofre F., Arturi F., Sciacqua A., Andreozzi F., Pietrangelo A., Sesti G., Perticone F., Violi F., Corrao S., Marengoni A., Tettamanti M., Pasina L., Franchi C., Miglio G., Ardoino I., Cantiero S., Prisco D., Silvestri E., Emmi G., Bettiol A., Mattioli I., Mazzetti M., Biolo G., Zanetti M., Bartelloni G., Zaccari M., Chiuch M., Martini I., Pirro M., Lupattelli G., Bianconi V., Alcidi R., Giotta A., Mannarino M. R., Girelli D., Busti F., Marchi G., Barbagallo M., Dominguez L., Beneduce V., Cacioppo F., Natoli G., Mularo S., Raspanti M., Argano C., Cavallaro F., Zoli M., Orio G., Magnolfi E., Serafini G., Brunori M., Lazzari I., Simili A., Fabio G., De Amicis M. M., Luca G., Scaramellini N., Stefano V., Leoni S., Seghezzi S., Di Mauro A. D., Maira D., Mancarella M., Lucchi T., Clerici M., Bonini G., Conti F., Prolo S., Fabrizi M., Martelengo M., Vigani G., Nicolini P., Sabatino A., Miceli E., Pisati M., Pitotti L., Antoci V., Cambie G., Pontremoli R., Beccati V., Nobili G., Leoncini G., Alberto J., Cattaneo F., Anastasio L., Sofia L., Carbone M., Cipollone F., Rossi I., Valeriani E., D'Ardes D., Cipollone A., Esposito L., Sestili S., Angelucci E., Mancuso G., Calipari D., Bartone M., Manetti R., Sircana M., Berria M., Delitala A., Muscaritoli M., Molfino A., Petrillo E., Giorgi A., Gracin C., Imbimbo G., Romanelli G., Volpini A., Lucente D., Manzoni F., Pirozzi A., Zucchelli A., Geneletti T., Picardi A., Bellelli G., Corsi M., Antonucci C., Sidoli C., Principato G., Bonfanti A., Szabo H., Mazzola P., Piazzoli A., Tassone B., De Falco A. B. T., Negro E., Brenna M., Trotta L., Fabris F., Bertozzi I., Bogoni G., Prandini T., Ratti F., Zurlo C., Cerruti L., Cosi E., Reni E., Manfredini R., Boari B., Tiseo R., Savrie C., Fabbian F., Paolisso G., Catalano C., Meo I., Sabba C., Suppressa P., De Vincenzo G. M., Comitangelo A., Amoruso E., Custodero C., Re G., Barnaba I., Schilardi A., Fenoglio L., Falcetta A., D'Aniano S., Tiraboschi S., Cespiati A., Oberti G., Sigon G., Cinque F., Colavolpe L., Curra J., Alletto F., Benzoni G., Peyvandi F., Rossio R., Colombo G., Agosti P., Pagliaro E., Semproni E., Canetta C., Monzani V., Savojardo V., Ceriani G., Folli C., Tognin T., Purrello F., Pino A., Piro S., Rozzini R., Falanga L., Boffelli S., Ferrandina C., Mazzeo F., Spazzini E., Cono G., Cesaroni G., Perri L., Guasti L., Rotunno F., Castiglioni L., Maresca A., Squizzato A., Campiotti L., Grossi A., Dentali F., Behnke V., Perticone M., Maio R., Scozzafava A., Condoleo V., Clausi E., Armentaro G., Panza A., Stanghellini V., Ruggeri E., Vecchio S., Benzoni I., Minisola S., Colangelo L., Cilli M., Labbadia G., Pepe J., Castellino P., Zanoli L., Gaudio A., Xourafa A., Spichetti C., Torre S., Gennaro A., Ballestrero A., Ferrando F., Gonella R., Cerminara D., Setti P., Traversa C., Scarsi C., Famularo G., Tarsitani P., Morretti T., Aglitti A., Giacco S., Firinu D., Costanzo G., Chessa S., Montalto G., Licata A., Rizzo A., Corica F., Basile G., Catalano A., Bellone F., Principato C., Cocuzza A., Mecocci P., Ruggiero C., Boccardi V., Meschi T., Ticinesi A., Nouvenne A., Pirisi M., Sola D., Bellan M., Quadri R., Larovere E., Novelli M., Simeone E., Scurti R., Tolloso F., Tarquini R., Valoriani A., Dolenti S., Vannini G., Volpi R., Bocchi P., Vignali A., Harari S., Lonati C., Napoli F., Aiello I., Salvatore T., Monaco L., Ricozzi C., Coviello F., Catalini C., Pilotto A., Indiano I., Gandolfo F., Gonella D., Nuti R., Valenti R., Ruvio M., Cappelli S., Palazzuoli A., Durante V., Tirotta D., Eusebi G., Tresoldi M., Bozzolo E., Damanti S., Porta M., Gino M., Pari B., and Pace E.
- Abstract
In this article the names of a few collaborators and some data in Table 5 were missing. It has been corrected. The original article has been corrected.
- Published
- 2023
328. Prescription appropriateness of anti-diabetes drugs in elderly patients hospitalized in a clinical setting: evidence from the REPOSI Register
- Author
-
Succurro, E, Novella, A, Nobili, A, Giofre, F, Arturi, F, Sciacqua, A, Andreozzi, F, Pietrangelo, A, Sesti, G, Perticone, F, Violi, F, Corrao, S, Marengoni, A, Tettamanti, M, Pasina, L, Franchi, C, Miglio, G, Ardoino, I, Cantiero, S, Prisco, D, Silvestri, E, Emmi, G, Bettiol, A, Mattioli, I, Mazzetti, M, Biolo, G, Zanetti, M, Bartelloni, G, Zaccari, M, Chiuch, M, Martini, I, Pirro, M, Lupattelli, G, Bianconi, V, Alcidi, R, Giotta, A, Mannarino, M, Girelli, D, Busti, F, Marchi, G, Barbagallo, M, Dominguez, L, Beneduce, V, Cacioppo, F, Natoli, G, Mularo, S, Raspanti, M, Argano, C, Cavallaro, F, Zoli, M, Orio, G, Magnolfi, E, Serafini, G, Brunori, M, Lazzari, I, Simili, A, Fabio, G, De Amicis, M, Luca, G, Scaramellini, N, Stefano, V, Leoni, S, Seghezzi, S, Di Mauro, A, Maira, D, Mancarella, M, Lucchi, T, Clerici, M, Bonini, G, Conti, F, Prolo, S, Fabrizi, M, Martelengo, M, Vigani, G, Nicolini, P, Sabatino, A, Miceli, E, Pisati, M, Pitotti, L, Antoci, V, Cambie, G, Pontremoli, R, Beccati, V, Nobili, G, Leoncini, G, Alberto, J, Cattaneo, F, Anastasio, L, Sofia, L, Carbone, M, Cipollone, F, Rossi, I, Valeriani, E, D'Ardes, D, Cipollone, A, Esposito, L, Sestili, S, Angelucci, E, Mancuso, G, Calipari, D, Bartone, M, Manetti, R, Sircana, M, Berria, M, Delitala, A, Muscaritoli, M, Molfino, A, Petrillo, E, Giorgi, A, Gracin, C, Imbimbo, G, Romanelli, G, Volpini, A, Lucente, D, Manzoni, F, Pirozzi, A, Zucchelli, A, Geneletti, T, Picardi, A, Bellelli, G, Corsi, M, Antonucci, C, Sidoli, C, Principato, G, Bonfanti, A, Szabo, H, Mazzola, P, Piazzoli, A, Tassone, B, De Falco, A, Negro, E, Brenna, M, Trotta, L, Fabris, F, Bertozzi, I, Bogoni, G, Prandini, T, Ratti, F, Zurlo, C, Cerruti, L, Cosi, E, Reni, E, Manfredini, R, Boari, B, Tiseo, R, Savrie, C, Fabbian, F, Paolisso, G, Catalano, C, Meo, I, Sabba, C, Suppressa, P, De Vincenzo, G, Comitangelo, A, Amoruso, E, Custodero, C, Re, G, Barnaba, I, Schilardi, A, Fenoglio, L, Falcetta, A, D'Aniano, S, Tiraboschi, S, Cespiati, A, Oberti, G, Sigon, G, Cinque, F, Colavolpe, L, Curra, J, Alletto, F, Benzoni, G, Peyvandi, F, Rossio, R, Colombo, G, Agosti, P, Pagliaro, E, Semproni, E, Canetta, C, Monzani, V, Savojardo, V, Ceriani, G, Folli, C, Tognin, T, Purrello, F, Pino, A, Piro, S, Rozzini, R, Falanga, L, Boffelli, S, Ferrandina, C, Mazzeo, F, Spazzini, E, Cono, G, Cesaroni, G, Perri, L, Guasti, L, Rotunno, F, Castiglioni, L, Maresca, A, Squizzato, A, Campiotti, L, Grossi, A, Dentali, F, Behnke, V, Perticone, M, Maio, R, Scozzafava, A, Condoleo, V, Clausi, E, Armentaro, G, Panza, A, Stanghellini, V, Ruggeri, E, Vecchio, S, Benzoni, I, Minisola, S, Colangelo, L, Cilli, M, Labbadia, G, Pepe, J, Castellino, P, Zanoli, L, Gaudio, A, Xourafa, A, Spichetti, C, Torre, S, Gennaro, A, Ballestrero, A, Ferrando, F, Gonella, R, Cerminara, D, Setti, P, Traversa, C, Scarsi, C, Famularo, G, Tarsitani, P, Morretti, T, Aglitti, A, Giacco, S, Firinu, D, Costanzo, G, Chessa, S, Montalto, G, Licata, A, Rizzo, A, Corica, F, Basile, G, Catalano, A, Bellone, F, Principato, C, Cocuzza, A, Mecocci, P, Ruggiero, C, Boccardi, V, Meschi, T, Ticinesi, A, Nouvenne, A, Pirisi, M, Sola, D, Bellan, M, Quadri, R, Larovere, E, Novelli, M, Simeone, E, Scurti, R, Tolloso, F, Tarquini, R, Valoriani, A, Dolenti, S, Vannini, G, Volpi, R, Bocchi, P, Vignali, A, Harari, S, Lonati, C, Napoli, F, Aiello, I, Salvatore, T, Monaco, L, Ricozzi, C, Coviello, F, Catalini, C, Pilotto, A, Indiano, I, Gandolfo, F, Gonella, D, Nuti, R, Valenti, R, Ruvio, M, Cappelli, S, Palazzuoli, A, Durante, V, Tirotta, D, Eusebi, G, Tresoldi, M, Bozzolo, E, Damanti, S, Porta, M, Gino, M, Pari, B, Pace, E, Succurro E., Novella A., Nobili A., Giofre F., Arturi F., Sciacqua A., Andreozzi F., Pietrangelo A., Sesti G., Perticone F., Violi F., Corrao S., Marengoni A., Tettamanti M., Pasina L., Franchi C., Miglio G., Ardoino I., Cantiero S., Prisco D., Silvestri E., Emmi G., Bettiol A., Mattioli I., Mazzetti M., Biolo G., Zanetti M., Bartelloni G., Zaccari M., Chiuch M., Martini I., Pirro M., Lupattelli G., Bianconi V., Alcidi R., Giotta A., Mannarino M. R., Girelli D., Busti F., Marchi G., Barbagallo M., Dominguez L., Beneduce V., Cacioppo F., Natoli G., Mularo S., Raspanti M., Argano C., Cavallaro F., Zoli M., Orio G., Magnolfi E., Serafini G., Brunori M., Lazzari I., Simili A., Fabio G., De Amicis M. M., Luca G., Scaramellini N., Stefano V., Leoni S., Seghezzi S., Di Mauro A. D., Maira D., Mancarella M., Lucchi T., Clerici M., Bonini G., Conti F., Prolo S., Fabrizi M., Martelengo M., Vigani G., Nicolini P., Sabatino A., Miceli E., Pisati M., Pitotti L., Antoci V., Cambie G., Pontremoli R., Beccati V., Nobili G., Leoncini G., Alberto J., Cattaneo F., Anastasio L., Sofia L., Carbone M., Cipollone F., Rossi I., Valeriani E., D'Ardes D., Cipollone A., Esposito L., Sestili S., Angelucci E., Mancuso G., Calipari D., Bartone M., Manetti R., Sircana M., Berria M., Delitala A., Muscaritoli M., Molfino A., Petrillo E., Giorgi A., Gracin C., Imbimbo G., Romanelli G., Volpini A., Lucente D., Manzoni F., Pirozzi A., Zucchelli A., Geneletti T., Picardi A., Bellelli G., Corsi M., Antonucci C., Sidoli C., Principato G., Bonfanti A., Szabo H., Mazzola P., Piazzoli A., Tassone B., De Falco A. B. T., Negro E., Brenna M., Trotta L., Fabris F., Bertozzi I., Bogoni G., Prandini T., Ratti F., Zurlo C., Cerruti L., Cosi E., Reni E., Manfredini R., Boari B., Tiseo R., Savrie C., Fabbian F., Paolisso G., Catalano C., Meo I., Sabba C., Suppressa P., De Vincenzo G. M., Comitangelo A., Amoruso E., Custodero C., Re G., Barnaba I., Schilardi A., Fenoglio L., Falcetta A., D'Aniano S., Tiraboschi S., Cespiati A., Oberti G., Sigon G., Cinque F., Colavolpe L., Curra J., Alletto F., Benzoni G., Peyvandi F., Rossio R., Colombo G., Agosti P., Pagliaro E., Semproni E., Canetta C., Monzani V., Savojardo V., Ceriani G., Folli C., Tognin T., Purrello F., Pino A., Piro S., Rozzini R., Falanga L., Boffelli S., Ferrandina C., Mazzeo F., Spazzini E., Cono G., Cesaroni G., Perri L., Guasti L., Rotunno F., Castiglioni L., Maresca A., Squizzato A., Campiotti L., Grossi A., Dentali F., Behnke V., Perticone M., Maio R., Scozzafava A., Condoleo V., Clausi E., Armentaro G., Panza A., Stanghellini V., Ruggeri E., Vecchio S., Benzoni I., Minisola S., Colangelo L., Cilli M., Labbadia G., Pepe J., Castellino P., Zanoli L., Gaudio A., Xourafa A., Spichetti C., Torre S., Gennaro A., Ballestrero A., Ferrando F., Gonella R., Cerminara D., Setti P., Traversa C., Scarsi C., Famularo G., Tarsitani P., Morretti T., Aglitti A., Giacco S., Firinu D., Costanzo G., Chessa S., Montalto G., Licata A., Rizzo A., Corica F., Basile G., Catalano A., Bellone F., Principato C., Cocuzza A., Mecocci P., Ruggiero C., Boccardi V., Meschi T., Ticinesi A., Nouvenne A., Pirisi M., Sola D., Bellan M., Quadri R., Larovere E., Novelli M., Simeone E., Scurti R., Tolloso F., Tarquini R., Valoriani A., Dolenti S., Vannini G., Volpi R., Bocchi P., Vignali A., Harari S., Lonati C., Napoli F., Aiello I., Salvatore T., Monaco L., Ricozzi C., Coviello F., Catalini C., Pilotto A., Indiano I., Gandolfo F., Gonella D., Nuti R., Valenti R., Ruvio M., Cappelli S., Palazzuoli A., Durante V., Tirotta D., Eusebi G., Tresoldi M., Bozzolo E., Damanti S., Porta M., Gino M., Pari B., Pace E., Succurro, E, Novella, A, Nobili, A, Giofre, F, Arturi, F, Sciacqua, A, Andreozzi, F, Pietrangelo, A, Sesti, G, Perticone, F, Violi, F, Corrao, S, Marengoni, A, Tettamanti, M, Pasina, L, Franchi, C, Miglio, G, Ardoino, I, Cantiero, S, Prisco, D, Silvestri, E, Emmi, G, Bettiol, A, Mattioli, I, Mazzetti, M, Biolo, G, Zanetti, M, Bartelloni, G, Zaccari, M, Chiuch, M, Martini, I, Pirro, M, Lupattelli, G, Bianconi, V, Alcidi, R, Giotta, A, Mannarino, M, Girelli, D, Busti, F, Marchi, G, Barbagallo, M, Dominguez, L, Beneduce, V, Cacioppo, F, Natoli, G, Mularo, S, Raspanti, M, Argano, C, Cavallaro, F, Zoli, M, Orio, G, Magnolfi, E, Serafini, G, Brunori, M, Lazzari, I, Simili, A, Fabio, G, De Amicis, M, Luca, G, Scaramellini, N, Stefano, V, Leoni, S, Seghezzi, S, Di Mauro, A, Maira, D, Mancarella, M, Lucchi, T, Clerici, M, Bonini, G, Conti, F, Prolo, S, Fabrizi, M, Martelengo, M, Vigani, G, Nicolini, P, Sabatino, A, Miceli, E, Pisati, M, Pitotti, L, Antoci, V, Cambie, G, Pontremoli, R, Beccati, V, Nobili, G, Leoncini, G, Alberto, J, Cattaneo, F, Anastasio, L, Sofia, L, Carbone, M, Cipollone, F, Rossi, I, Valeriani, E, D'Ardes, D, Cipollone, A, Esposito, L, Sestili, S, Angelucci, E, Mancuso, G, Calipari, D, Bartone, M, Manetti, R, Sircana, M, Berria, M, Delitala, A, Muscaritoli, M, Molfino, A, Petrillo, E, Giorgi, A, Gracin, C, Imbimbo, G, Romanelli, G, Volpini, A, Lucente, D, Manzoni, F, Pirozzi, A, Zucchelli, A, Geneletti, T, Picardi, A, Bellelli, G, Corsi, M, Antonucci, C, Sidoli, C, Principato, G, Bonfanti, A, Szabo, H, Mazzola, P, Piazzoli, A, Tassone, B, De Falco, A, Negro, E, Brenna, M, Trotta, L, Fabris, F, Bertozzi, I, Bogoni, G, Prandini, T, Ratti, F, Zurlo, C, Cerruti, L, Cosi, E, Reni, E, Manfredini, R, Boari, B, Tiseo, R, Savrie, C, Fabbian, F, Paolisso, G, Catalano, C, Meo, I, Sabba, C, Suppressa, P, De Vincenzo, G, Comitangelo, A, Amoruso, E, Custodero, C, Re, G, Barnaba, I, Schilardi, A, Fenoglio, L, Falcetta, A, D'Aniano, S, Tiraboschi, S, Cespiati, A, Oberti, G, Sigon, G, Cinque, F, Colavolpe, L, Curra, J, Alletto, F, Benzoni, G, Peyvandi, F, Rossio, R, Colombo, G, Agosti, P, Pagliaro, E, Semproni, E, Canetta, C, Monzani, V, Savojardo, V, Ceriani, G, Folli, C, Tognin, T, Purrello, F, Pino, A, Piro, S, Rozzini, R, Falanga, L, Boffelli, S, Ferrandina, C, Mazzeo, F, Spazzini, E, Cono, G, Cesaroni, G, Perri, L, Guasti, L, Rotunno, F, Castiglioni, L, Maresca, A, Squizzato, A, Campiotti, L, Grossi, A, Dentali, F, Behnke, V, Perticone, M, Maio, R, Scozzafava, A, Condoleo, V, Clausi, E, Armentaro, G, Panza, A, Stanghellini, V, Ruggeri, E, Vecchio, S, Benzoni, I, Minisola, S, Colangelo, L, Cilli, M, Labbadia, G, Pepe, J, Castellino, P, Zanoli, L, Gaudio, A, Xourafa, A, Spichetti, C, Torre, S, Gennaro, A, Ballestrero, A, Ferrando, F, Gonella, R, Cerminara, D, Setti, P, Traversa, C, Scarsi, C, Famularo, G, Tarsitani, P, Morretti, T, Aglitti, A, Giacco, S, Firinu, D, Costanzo, G, Chessa, S, Montalto, G, Licata, A, Rizzo, A, Corica, F, Basile, G, Catalano, A, Bellone, F, Principato, C, Cocuzza, A, Mecocci, P, Ruggiero, C, Boccardi, V, Meschi, T, Ticinesi, A, Nouvenne, A, Pirisi, M, Sola, D, Bellan, M, Quadri, R, Larovere, E, Novelli, M, Simeone, E, Scurti, R, Tolloso, F, Tarquini, R, Valoriani, A, Dolenti, S, Vannini, G, Volpi, R, Bocchi, P, Vignali, A, Harari, S, Lonati, C, Napoli, F, Aiello, I, Salvatore, T, Monaco, L, Ricozzi, C, Coviello, F, Catalini, C, Pilotto, A, Indiano, I, Gandolfo, F, Gonella, D, Nuti, R, Valenti, R, Ruvio, M, Cappelli, S, Palazzuoli, A, Durante, V, Tirotta, D, Eusebi, G, Tresoldi, M, Bozzolo, E, Damanti, S, Porta, M, Gino, M, Pari, B, Pace, E, Succurro E., Novella A., Nobili A., Giofre F., Arturi F., Sciacqua A., Andreozzi F., Pietrangelo A., Sesti G., Perticone F., Violi F., Corrao S., Marengoni A., Tettamanti M., Pasina L., Franchi C., Miglio G., Ardoino I., Cantiero S., Prisco D., Silvestri E., Emmi G., Bettiol A., Mattioli I., Mazzetti M., Biolo G., Zanetti M., Bartelloni G., Zaccari M., Chiuch M., Martini I., Pirro M., Lupattelli G., Bianconi V., Alcidi R., Giotta A., Mannarino M. R., Girelli D., Busti F., Marchi G., Barbagallo M., Dominguez L., Beneduce V., Cacioppo F., Natoli G., Mularo S., Raspanti M., Argano C., Cavallaro F., Zoli M., Orio G., Magnolfi E., Serafini G., Brunori M., Lazzari I., Simili A., Fabio G., De Amicis M. M., Luca G., Scaramellini N., Stefano V., Leoni S., Seghezzi S., Di Mauro A. D., Maira D., Mancarella M., Lucchi T., Clerici M., Bonini G., Conti F., Prolo S., Fabrizi M., Martelengo M., Vigani G., Nicolini P., Sabatino A., Miceli E., Pisati M., Pitotti L., Antoci V., Cambie G., Pontremoli R., Beccati V., Nobili G., Leoncini G., Alberto J., Cattaneo F., Anastasio L., Sofia L., Carbone M., Cipollone F., Rossi I., Valeriani E., D'Ardes D., Cipollone A., Esposito L., Sestili S., Angelucci E., Mancuso G., Calipari D., Bartone M., Manetti R., Sircana M., Berria M., Delitala A., Muscaritoli M., Molfino A., Petrillo E., Giorgi A., Gracin C., Imbimbo G., Romanelli G., Volpini A., Lucente D., Manzoni F., Pirozzi A., Zucchelli A., Geneletti T., Picardi A., Bellelli G., Corsi M., Antonucci C., Sidoli C., Principato G., Bonfanti A., Szabo H., Mazzola P., Piazzoli A., Tassone B., De Falco A. B. T., Negro E., Brenna M., Trotta L., Fabris F., Bertozzi I., Bogoni G., Prandini T., Ratti F., Zurlo C., Cerruti L., Cosi E., Reni E., Manfredini R., Boari B., Tiseo R., Savrie C., Fabbian F., Paolisso G., Catalano C., Meo I., Sabba C., Suppressa P., De Vincenzo G. M., Comitangelo A., Amoruso E., Custodero C., Re G., Barnaba I., Schilardi A., Fenoglio L., Falcetta A., D'Aniano S., Tiraboschi S., Cespiati A., Oberti G., Sigon G., Cinque F., Colavolpe L., Curra J., Alletto F., Benzoni G., Peyvandi F., Rossio R., Colombo G., Agosti P., Pagliaro E., Semproni E., Canetta C., Monzani V., Savojardo V., Ceriani G., Folli C., Tognin T., Purrello F., Pino A., Piro S., Rozzini R., Falanga L., Boffelli S., Ferrandina C., Mazzeo F., Spazzini E., Cono G., Cesaroni G., Perri L., Guasti L., Rotunno F., Castiglioni L., Maresca A., Squizzato A., Campiotti L., Grossi A., Dentali F., Behnke V., Perticone M., Maio R., Scozzafava A., Condoleo V., Clausi E., Armentaro G., Panza A., Stanghellini V., Ruggeri E., Vecchio S., Benzoni I., Minisola S., Colangelo L., Cilli M., Labbadia G., Pepe J., Castellino P., Zanoli L., Gaudio A., Xourafa A., Spichetti C., Torre S., Gennaro A., Ballestrero A., Ferrando F., Gonella R., Cerminara D., Setti P., Traversa C., Scarsi C., Famularo G., Tarsitani P., Morretti T., Aglitti A., Giacco S., Firinu D., Costanzo G., Chessa S., Montalto G., Licata A., Rizzo A., Corica F., Basile G., Catalano A., Bellone F., Principato C., Cocuzza A., Mecocci P., Ruggiero C., Boccardi V., Meschi T., Ticinesi A., Nouvenne A., Pirisi M., Sola D., Bellan M., Quadri R., Larovere E., Novelli M., Simeone E., Scurti R., Tolloso F., Tarquini R., Valoriani A., Dolenti S., Vannini G., Volpi R., Bocchi P., Vignali A., Harari S., Lonati C., Napoli F., Aiello I., Salvatore T., Monaco L., Ricozzi C., Coviello F., Catalini C., Pilotto A., Indiano I., Gandolfo F., Gonella D., Nuti R., Valenti R., Ruvio M., Cappelli S., Palazzuoli A., Durante V., Tirotta D., Eusebi G., Tresoldi M., Bozzolo E., Damanti S., Porta M., Gino M., Pari B., and Pace E.
- Abstract
Diabetes is an increasing global health burden with the highest prevalence (24.0%) observed in elderly people. Older diabetic adults have a greater risk of hospitalization and several geriatric syndromes than older nondiabetic adults. For these conditions, special care is required in prescribing therapies including anti- diabetes drugs. Aim of this study was to evaluate the appropriateness and the adherence to safety recommendations in the prescriptions of glucose-lowering drugs in hospitalized elderly patients with diabetes. Data for this cross-sectional study were obtained from the REgistro POliterapie–Società Italiana Medicina Interna (REPOSI) that collected clinical information on patients aged ≥ 65 years acutely admitted to Italian internal medicine and geriatric non-intensive care units (ICU) from 2010 up to 2019. Prescription appropriateness was assessed according to the 2019 AGS Beers Criteria and anti-diabetes drug data sheets.Among 5349 patients, 1624 (30.3%) had diagnosis of type 2 diabetes. At admission, 37.7% of diabetic patients received treatment with metformin, 37.3% insulin therapy, 16.4% sulfonylureas, and 11.4% glinides. Surprisingly, only 3.1% of diabetic patients were treated with new classes of anti- diabetes drugs. According to prescription criteria, at admission 15.4% of patients treated with metformin and 2.6% with sulfonylureas received inappropriately these treatments. At discharge, the inappropriateness of metformin therapy decreased (10.2%, P < 0.0001). According to Beers criteria, the inappropriate prescriptions of sulfonylureas raised to 29% both at admission and at discharge. This study shows a poor adherence to current guidelines on diabetes management in hospitalized elderly people with a high prevalence of inappropriate use of sulfonylureas according to the Beers criteria.
- Published
- 2023
329. In-Plane Nanowire Growth of Topological Crystalline Insulator Pb1−xSnxTe
- Author
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Schellingerhout, S, Bergamaschini, R, Verheijen, M, Montalenti, F, Miglio, L, Bakkers, E, Schellingerhout S. G., Bergamaschini R., Verheijen M. A., Montalenti F., Miglio L., Bakkers E. P. A. M., Schellingerhout, S, Bergamaschini, R, Verheijen, M, Montalenti, F, Miglio, L, Bakkers, E, Schellingerhout S. G., Bergamaschini R., Verheijen M. A., Montalenti F., Miglio L., and Bakkers E. P. A. M.
- Abstract
Predicted topological crystalline insulators such as Pb1−xSnxTe are an interesting candidate for applications in quantum technology, as they can host spin-polarized surface states. Moreover, in the nanowire geometry, a quasi-1D system can be realized with potential applications exploiting Majorana fermions. Herein, the selective area growth of Pb1−xSnxTe islands and nanowires over the full range of x is demonstrated, and their in-depth growth dynamics and faceting are analyzed. By transmission electron microscopy, the single-crystalline and defect-free nature of the grown material and the homogeneous, controllable Pb/Sn ratio in the nanowires is confirmed. With support of phase-field growth simulations, it is shown that the crystal faceting mainly follows the driving force of surface energy minimization, favoring the lowest energy {200} surfaces. A kinetic enhancement of adatom incorporation on {110} facets is recognized to limit their extension with respect to {200} and {111} facets. After inspecting all possible in-plane orientations, we identify the <110> directions as the optimal candidate for the growth of high-quality and perfectly straight Pb1−xSnxTe nanowires, enabling the design of complex networks due to their threefold symmetry. This work opens the way to systematic transport investigation of the carrier density in Pb1−xSnxTe nanowires and can facilitate further optimization of the Pb1−xSnxTe system.
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- 2023
330. Hexagonal Diamond phase of Si and Ge by nanoindentation
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Rovaris, F, Ge, G, Marzegalli, A, Miglio, L, Scalise, E, Fabrizio Rovaris, Guojia Ge, Anna Marzegalli, Leonida Miglio, Emilio Scalise, Rovaris, F, Ge, G, Marzegalli, A, Miglio, L, Scalise, E, Fabrizio Rovaris, Guojia Ge, Anna Marzegalli, Leonida Miglio, and Emilio Scalise
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- 2023
331. Photonic Properties of Self-Assembled Semiconductor Microstructures
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Pedrini, J, Colombo, I, Minazzi, P, Barzaghi, A, Miglio, L, Isella, G, Pezzoli, F, Jacopo Pedrini, Ian Colombo, Pietro Minazzi, Andrea Barzaghi, Leonida Miglio, Giovanni Isella, Fabio Pezzoli, Pedrini, J, Colombo, I, Minazzi, P, Barzaghi, A, Miglio, L, Isella, G, Pezzoli, F, Jacopo Pedrini, Ian Colombo, Pietro Minazzi, Andrea Barzaghi, Leonida Miglio, Giovanni Isella, and Fabio Pezzoli
- Published
- 2023
332. For Us, but Not to Us: Essays on Creation, Covenant, and Context in Honor of John H. Walton
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Adam E. Miglio, Caryn A. Reeder, Joshua T. Walton, Kenneth C. Way and Adam E. Miglio, Caryn A. Reeder, Joshua T. Walton, Kenneth C. Way
- Published
- 2020
333. Stellar Spin-Orbit Misalignment in a Multiplanet System
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Huber, Daniel, Carter, Joshua A., Barbieri, Mauro, Miglio, Andrea, Deck, Katherine M., Fabrycky, Daniel C., Montet, Benjamin T., Buchhave, Lars A., Chaplin, William J., Hekker, Saskia, Montalbán, Josefina, Sanchis-Ojeda, Roberto, Basu, Sarbani, Bedding, Timothy R., Campante, Tiago L., Christensen-Dalsgaard, Joergen, Elsworth, Yvonne P., Stello, Dennis, Arentoft, Torben, Ford, Eric B., Gilliland, Ronald L., Handberg, Rasmus, Howard, Andrew W., Isaacson, Howard, Johnson, John Asher, Karoff, Christoffer, Kawaler, Steven D., Kjeldsen, Hans, Latham, David W., Lund, Mikkel N., Lundkvist, Mia, Marcy, Geoffrey W., Metcalfe, Travis S., Aguirre, Victor Silva, and Winn, Joshua N.
- Subjects
Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
Stars hosting hot Jupiters are often observed to have high obliquities, whereas stars with multiple co-planar planets have been seen to have low obliquities. This has been interpreted as evidence that hot-Jupiter formation is linked to dynamical disruption, as opposed to planet migration through a protoplanetary disk. We used asteroseismology to measure a large obliquity for Kepler-56, a red giant star hosting two transiting co-planar planets. These observations show that spin-orbit misalignments are not confined to hot-Jupiter systems. Misalignments in a broader class of systems had been predicted as a consequence of torques from wide-orbiting companions, and indeed radial-velocity measurements revealed a third companion in a wide orbit in the Kepler-56 system., Comment: Accepted for publication in Science, published online on October 17 2013; PDF includes main article and supplementary materials (65 pages, 27 figures, 7 tables); v2: small correction to author list
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- 2013
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334. Asteroseismic fundamental properties of solar-type stars observed by the NASA Kepler Mission
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Chaplin, W. J., Basu, S., Huber, D., Serenelli, A, Casagrande, L., Aguirre, V. Silva, Ball, W. H., Creevey, O. L., Gizon, L., Handberg, R., Karoff, C., Lutz, R., Marques, J. P., Miglio, A., Stello, D., Suran, M. D., Pricopi, D., Metcalfe, T. S., Monteiro, M. J. P. F. G., Molenda-Zakowicz, J., Appourchaux, T., Christensen-Dalsgaard, J., Elsworth, Y., Garcia, R. A., Houdek, G., Kjeldsen, H., Bonanno, A., Campante, T. L., Corsaro, E., Gaulme, P., Hekker, S., Mathur, S., Mosser, B., Regulo, C., and Salabert, D.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
We use asteroseismic data obtained by the NASA Kepler Mission to estimate the fundamental properties of more than 500 main-sequence and sub-giant stars. Data obtained during the first 10 months of Kepler science operations were used for this work, when these solar-type targets were observed for one month each in a survey mode. Stellar properties have been estimated using two global asteroseismic parameters and complementary photometric and spectroscopic data. Homogeneous sets of effective temperatures were available for the entire ensemble from complementary photometry; spectroscopic estimates of T_eff and [Fe/H] were available from a homogeneous analysis of ground-based data on a subset of 87 stars. [Abbreviated version... see paper for full abstract.], Comment: Accepted for publication in ApJS; 90 pages, 22 figures, 6 tables. Units on rho in tables now listed correctly as rho(Sun)
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- 2013
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335. The PLATO 2.0 Mission
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Rauer, H., Catala, C., Aerts, C., Appourchaux, T., Benz, W., Brandeker, A., Christensen-Dalsgaard, J., Deleuil, M., Gizon, L., Goupil, M. -J., Güdel, M., Janot-Pacheco, E., Mas-Hesse, M., Pagano, I., Piotto, G., Pollacco, D., Santos, N. C., Smith, A., -C., J., Suárez, Szabó, R., Udry, S., Adibekyan, V., Alibert, Y., Almenara, J. -M., Amaro-Seoane, P., Eiff, M. Ammler-von, Asplund, M., Antonello, E., Ball, W., Barnes, S., Baudin, F., Belkacem, K., Bergemann, M., Bihain, G., Birch, A. C., Bonfils, X., Boisse, I., Bonomo, A. S., Borsa, F., Brandão, I. M., Brocato, E., Brun, S., Burleigh, M., Burston, R., Cabrera, J., Cassisi, S., Chaplin, W., Charpinet, S., Chiappini, C., Church, R. P., Csizmadia, Sz., Cunha, M., Damasso, M., Davies, M. B., Deeg, H. J., DÍaz, R. F., Dreizler, S., Dreyer, C., Eggenberger, P., Ehrenreich, D., Eigmüller, P., Erikson, A., Farmer, R., Feltzing, S., Fialho, F. de Oliveira, Figueira, P., Forveille, T., Fridlund, M., García, R. A., Giommi, P., Giuffrida, G., Godolt, M., da Silva, J. Gomes, Granzer, T., Grenfell, J. L., Grotsch-Noels, A., Günther, E., Haswell, C. A., Hatzes, A. P., Hébrard, G., Hekker, S., Helled, R., Heng, K., Jenkins, J. M., Johansen, A., Khodachenko, M. L., Kislyakova, K. G., Kley, W., Kolb, U., Krivova, N., Kupka, F., Lammer, H., Lanza, A. F., Lebreton, Y., Magrin, D., Marcos-Arenal, P., Marrese, P. M., Marques, J. P., Martins, J., Mathis, S., Mathur, S., Messina, S., Miglio, A., Montalban, J., Montalto, M., Monteiro, M. J. P. F. G., Moradi, H., Moravveji, E., Mordasini, C., Morel, T., Mortier, A., Nascimbeni, V., Nelson, R. P., Nielsen, M. B., Noack, L., Norton, A. J., Ofir, A., Oshagh, M., Ouazzani, R. -M., Pápics, P., Parro, V. C., Petit, P., Plez, B., Poretti, E., Quirrenbach, A., Ragazzoni, R., Raimondo, G., Rainer, M., Reese, D. R., Redmer, R., Reffert, S., Rojas-Ayala, B., Roxburgh, I. W., Salmon, S., Santerne, A., Schneider, J., Schou, J., Schuh, S., Schunker, H., Silva-Valio, A., Silvotti, R., Skillen, I., Snellen, I., Sohl, F., Sousa, S. G., Sozzetti, A., Stello, D., Strassmeier, K. G., Švanda, M., Szabó, Gy. M., Tkachenko, A., Valencia, D., van Grootel, V., Vauclair, S. D., Ventura, P., Wagner, F. W., Walton, N. A., Weingrill, J., Werner, S. C., Wheatley, P. J., and Zwintz, K.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
PLATO 2.0 has recently been selected for ESA's M3 launch opportunity (2022/24). Providing accurate key planet parameters (radius, mass, density and age) in statistical numbers, it addresses fundamental questions such as: How do planetary systems form and evolve? Are there other systems with planets like ours, including potentially habitable planets? The PLATO 2.0 instrument consists of 34 small aperture telescopes (32 with 25 sec readout cadence and 2 with 2.5 sec candence) providing a wide field-of-view (2232 deg2) and a large photometric magnitude range (4-16 mag). It focusses on bright (4-11 mag) stars in wide fields to detect and characterize planets down to Earth-size by photometric transits, whose masses can then be determined by ground-based radial-velocity follow-up measurements. Asteroseismology will be performed for these bright stars to obtain highly accurate stellar parameters, including masses and ages. The combination of bright targets and asteroseismology results in high accuracy for the bulk planet parameters: 2%, 4-10% and 10% for planet radii, masses and ages, respectively. The planned baseline observing strategy includes two long pointings (2-3 years) to detect and bulk characterize planets reaching into the habitable zone (HZ) of solar-like stars and an additional step-and-stare phase to cover in total about 50% of the sky. PLATO 2.0 will observe up to 1,000,000 stars and detect and characterize hundreds of small planets, and thousands of planets in the Neptune to gas giant regime out to the HZ. It will therefore provide the first large-scale catalogue of bulk characterized planets with accurate radii, masses, mean densities and ages. This catalogue will include terrestrial planets at intermediate orbital distances, where surface temperatures are moderate. Coverage of this parameter range with statistical numbers of bulk characterized planets is unique to PLATO 2.0., Comment: 63 pages, 17 figures, submitted to Experimental Astronomy (ExA)
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- 2013
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336. An observational asteroseismic study of the pulsating B-stars in the open cluster NGC 884
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Saesen, S., Briquet, M., Aerts, C., Miglio, A., and Carrier, F.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Recent progress in the seismic interpretation of field {\beta} Cep stars has resulted in improvements of the physical description in the stellar structure and evolution model computations of massive stars. Further asteroseismic constraints can be obtained from studying ensembles of stars in a young open cluster, which all have similar age, distance and chemical composition. We present an observational asteroseismic study based on the discovery of numerous multi-periodic and mono-periodic B-stars in the open cluster NGC 884. Our study illustrates the current status of ensemble asteroseismology of a young open cluster., Comment: 2 pages, proceedings of the IAU Symposium No. 301 (2013), "Precision Asteroseismology" (Wroclaw), W. Chaplin, J. Guzik, G. Handler & A. Pigulski (eds.)
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- 2013
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337. Kepler White Paper: Asteroseismology of Solar-Like Oscillators in a 2-Wheel Mission
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Chaplin, W. J, Kjeldsen, H., Christensen-Dalsgaard, J., Gilliland, R. L., Kawaler, S. D., Basu, S., De Ridder, J., Huber, D., Arentoft, T., Schou, J., Garcia, R. A., Metcalfe, T. S., Brogaard, K., Campante, T. L., Elsworth, Y., Miglio, A., Appourchaux, T., Bedding, T. R., Hekker, S., Houdek, G., Karoff, C., Molenda-Zakowicz, J., Monteiro, M. J. P. F. G., Aguirre, V. Silva, Stello, D., Ball, W., Beck, P. G., Birch, A. C., Buzasi, D. L., Casagrande, L., Cellier, T., Corsaro, E., Creevey, O. L., Davies, G. R., Deheuvels, S., Dogan, G., Gizon, L., Grundahl, F., Guzik, J., Handberg, R., Jimenez, A., Kallinger, T., Lund, M. N., Lundkvist, M., Mathis, S., Mathur, S., Mazumdar, A., Mosser, B., Neiner, C., Nielsen, M. B., Palle, P. L., Pinsonneault, M. H., Salabert, D., Serenelli, A. M., Shunker, H., and White, T. R.
- Subjects
Astrophysics - Solar and Stellar Astrophysics - Abstract
We comment on the potential for continuing asteroseismology of solar-type and red-giant stars in a 2-wheel Kepler Mission. Our main conclusion is that by targeting stars in the ecliptic it should be possible to perform high-quality asteroseismology, as long as favorable scenarios for 2-wheel pointing performance are met. Targeting the ecliptic would potentially facilitate unique science that was not possible in the nominal Mission, notably from the study of clusters that are significantly brighter than those in the Kepler field. Our conclusions are based on predictions of 2-wheel observations made by a space photometry simulator, with information provided by the Kepler Project used as input to describe the degraded pointing scenarios. We find that elevated levels of frequency-dependent noise, consistent with the above scenarios, would have a significant negative impact on our ability to continue asteroseismic studies of solar-like oscillators in the Kepler field. However, the situation may be much more optimistic for observations in the ecliptic, provided that pointing resets of the spacecraft during regular desaturations of the two functioning reaction wheels are accurate at the < 1 arcsec level. This would make it possible to apply a post-hoc analysis that would recover most of the lost photometric precision. Without this post-hoc correction---and the accurate re-pointing it requires---the performance would probably be as poor as in the Kepler-field case. Critical to our conclusions for both fields is the assumed level of pointing noise (in the short-term jitter and the longer-term drift). We suggest that further tests will be needed to clarify our results once more detail and data on the expected pointing performance becomes available, and we offer our assistance in this work., Comment: NASA Kepler Mission White Paper; 10 pages, 2 figures
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- 2013
338. Fundamental stellar properties from asteroseismology
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Aguirre, V. Silva, Casagrande, L., and Miglio, A.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
Accurate characterization of stellar populations is of prime importance to correctly understand the formation and evolution process of our Galaxy. The field of asteroseismology has been particularly successful in such an endeavor providing fundamental parameters for large samples of stars in different evolutionary phases. We present our results on determinations of masses, radii, and distances of stars in the CoRoT and Kepler fields, showing that we can map and date different regions of the galactic disk and distinguish gradients in the distribution of stellar properties at different heights. We further review how asteroseismic determinations can produce a unique set of constraints, including ages, outside the solar neighborhood for galactic chemical evolution models., Comment: 6 pages, 3 figures. To appear in Proceedings IAU Symposium No. 298, "Setting the scene for Gaia and LAMOST", eds. S. Feltzing, G. Zhao, N. A. Walton, and P. A. Whitelock
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- 2013
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339. Pulsating B-type stars in the open cluster NGC 884: frequencies, mode identification and asteroseismology
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Saesen, S., Briquet, M., Aerts, C., Miglio, A., and Carrier, F.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Recent progress in the seismic interpretation of field beta Cep stars has resulted in improvements of the physics in the stellar structure and evolution models of massive stars. Further asteroseismic constraints can be obtained from studying ensembles of stars in a young open cluster, which all have similar age, distance and chemical composition. We present an observational asteroseismology study based on the discovery of numerous multi-periodic and mono-periodic B-stars in the open cluster NGC 884. We describe a thorough investigation of the pulsational properties of all B-type stars in the cluster. Overall, our detailed frequency analysis resulted in 115 detected frequencies in 65 stars. We found 36 mono-periodic, 16 bi-periodic, 10 tri-periodic, and 2 quadru-periodic stars and one star with 9 independent frequencies. We also derived the amplitudes and phases of all detected frequencies in the U, B, V and I filter, if available. We achieved unambiguous identifications of the mode degree for twelve of the detected frequencies in nine of the pulsators. Imposing the identified degrees and measured frequencies of the radial, dipole and quadrupole modes of five pulsators led to a seismic cluster age estimate of log(age/yr) =7.12-7.28 from a comparison with stellar models. Our study is a proof-of-concept for and illustrates the current status of ensemble asteroseismology of a young open cluster., Comment: Accepted for publication in The Astronomical Journal, 40 pages, 9 figures, 5 tables. The full appendix (online material) is appended to the article and contains 26 pages, 1 large table and 106 figures
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- 2013
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340. Multi-periodic pulsations of a stripped red giant star in an eclipsing binary
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Maxted, Pierre F. L., Serenelli, Aldo M., Miglio, Andrea, Marsh, Thomas R., Heber, Ulrich, Dhillon, Vikram S., Littlefair, Stuart, Copperwheat, Chris, Smalley, Barry, Breedt, Elmé, and Schaffenroth, Veronika
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Low mass white dwarfs are the remnants of disrupted red giant stars in binary millisecond pulsars and other exotic binary star systems. Some low mass white dwarfs cool rapidly, while others stay bright for millions of years due to stable fusion in thick surface hydrogen layers. This dichotomy is not well understood so their potential use as independent clocks to test the spin-down ages of pulsars or as probes of the extreme environments in which low mass white dwarfs form cannot be fully exploited. Here we present precise mass and radius measurements for the precursor to a low mass white dwarf. We find that only models in which this star has a thick hydrogen envelope can match the strong constraints provided by our new observations. Very cool low mass white dwarfs must therefore have lost their thick hydrogen envelopes by irradiation from pulsar companions or by episodes of unstable hydrogen fusion (shell flashes). We also find that this low mass white dwarf precursor is a new type of pulsating star. The observed pulsation frequencies are sensitive to internal processes that determine whether this star will undergo shell flashes., Comment: 15 pages, 3 figures. Published in Nature
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- 2013
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341. Germanium crystals on silicon show their light
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Pezzoli, F., Isa, F., Isella, G., Falub, C. V., Kreiliger, T., Salvalaglio, M., Bergamaschini, R., Grilli, E., Guzzi, M., von Kaenel, H., and Miglio, Leo
- Subjects
Condensed Matter - Materials Science - Abstract
Germanium and silicon-germanium alloys have found entry into Si technology thanks to their compatibility with Si processing and their ability to tailor electronic properties by strain and band-gap engineering. Germanium's potential to extend Si functionalities, as exemplified by lasing action of strained-Ge on Si substrates, has brought the material back to attention. Yet despite these advances, non-radiative transitions, induced by crystal defects originating from the Ge/Si interface, continue to be a serious bottleneck. Here we demonstrate the drastic emission enhancement achieved via control and mitigation over the parasitic activity of defects in micronscale Ge/Si crystals. We unravel how defects affect interband luminescence and minimize their influence by controlling carrier diffusion with band-gap-engineered reflectors. We finally extended this approach designing efficient quantum well emitters. Our results pave the way for the large-scale implementation of advanced electronic and photonic structures unaffected by the ubiquitous presence of defects developed at epitaxial interfaces.
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- 2013
342. A sub-Mercury-sized exoplanet
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Barclay, Thomas, Rowe, Jason F., Lissauer, Jack J., Huber, Daniel, Fressin, Francois, Howell, Steve B., Bryson, Stephen T., Chaplin, William J., Désert, Jean-Michel, Lopez, Eric D., Marcy, Geoffrey W., Mullally, Fergal, Ragozzine, Darin, Torres, Guillermo, Adams, Elisabeth R., Agol, Eric, Barrado, David, Basu, Sarbani, Bedding, Timothy R., Buchhave, Lars A., Charbonneau, David, Christiansen, Jessie L., Christensen-Dalsgaard, Jørgen, Ciardi, David, Cochran, William D., Dupree, Andrea K., Elsworth, Yvonne, Everett, Mark, Fischer, Debra A., Ford, Eric B., Fortney, Jonathan J., Geary, John C., Haas, Michael R., Handberg, Rasmus, Hekker, Saskia, Henze, Christopher E., Horch, Elliott, Howard, Andrew W., Hunter, Roger C., Isaacson, Howard, Jenkins, Jon M., Karoff, Christoffer, Kawaler, Steven D., Kjeldsen, Hans, Klaus, Todd C., Latham, David W., Li, Jie, Lillo-Box, Jorge, Lund, Mikkel N., Lundkvist, Mia, Metcalfe, Travis S., Miglio, Andrea, Morris, Robert L., Quintana, Elisa V., Stello, Dennis, Smith, Jeffrey C., Still, Martin, and Thompson, Susan E.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
Since the discovery of the first exoplanet we have known that other planetary systems can look quite unlike our own. However, until recently we have only been able to probe the upper range of the planet size distribution. The high precision of the Kepler space telescope has allowed us to detect planets that are the size of Earth and somewhat smaller, but no previous planets have been found that are smaller than those we see in our own Solar System. Here we report the discovery of a planet significantly smaller than Mercury. This tiny planet is the innermost of three planets that orbit the Sun-like host star, which we have designated Kepler-37. Owing to its extremely small size, similar to that of Earth's Moon, and highly irradiated surface, Kepler-37b is probably a rocky planet with no atmosphere or water, similar to Mercury., Comment: Accepted and published in Nature (2013 Feb 28). This is the submitted version of paper, merged with the Supplementary Information
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- 2013
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343. Low Hole Effective Mass p-type Transparent Conducting Oxides: Identification and Design Principles
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Hautier, Geoffroy, Miglio, Anna, Ceder, Gerbrand, Rignanese, Gian-Marco, and Gonze, Xavier
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Condensed Matter - Materials Science - Abstract
The development of high performance transparent conducting oxides (TCOs) is critical to many technologies from transparent electronics to solar cells. While n-type TCOs are present in many devices, current p-type TCOs are not largely commercialized as they exhibit much lower carrier mobilities, due to the large hole effective masses of most oxides. Here, we conduct a high-throughput computational search on thousands of binary and ternary oxides and identify several highly promising compounds displaying exceptionally low hole effective masses (up to an order of magnitude lower than state of the art p-type TCOs) as well as wide band gaps. In addition to the discovery of specific compounds, the chemical rationalization of our findings opens new directions, beyond current Cu-based chemistries, for the design and development of future p-type TCOs.
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- 2013
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344. Asteroseismology of Solar-Type and Red-Giant Stars
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Chaplin, William J. and Miglio, Andrea
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Astrophysics - Solar and Stellar Astrophysics - Abstract
We are entering a golden era for stellar physics driven by satellite and telescope observations of unprecedented quality and scope. New insights on stellar evolution and stellar interiors physics are being made possible by asteroseismology, the study of stars by the observation of natural, resonant oscillations. Asteroseismology is proving to be particularly significant for the study of solar-type and red-giant stars. These stars show rich spectra of solar-like oscillations, which are excited and intrinsically damped by turbulence in the outermost layers of the convective envelopes. In this review we discuss the current state of the field, with a particular emphasis on recent advances provided by the Kepler and CoRoT space missions and the wider significance to astronomy of the results from asteroseismology, such as stellar populations studies and exoplanet studies., Comment: The following paper will appear in the 2013 volume of Annual Reviews of Astronomy and Astrophysics (88 pages, 7 figures; references updated; further corrections to typos during galley-proof review)
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- 2013
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345. Band widths and gaps from the Tran-Blaha functional : Comparison with many-body perturbation theory
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Waroquiers, David, Lherbier, Aurélien, Miglio, Anna, Stankovski, Martin, Poncé, Samuel, Oliveira, Micael J. T., Giantomassi, Matteo, Rignanese, Gian-Marco, and Gonze, Xavier
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Condensed Matter - Materials Science ,Condensed Matter - Other Condensed Matter - Abstract
For a set of ten crystalline materials (oxides and semiconductors), we compute the electronic band structures using the Tran-Blaha [Phys. Rev. Lett. 102, 226401 (2009)] (TB09) functional. The band widths and gaps are compared with those from the local-density approximation (LDA) functional, many-body perturbation theory (MBPT), and experiments. At the density-functional theory (DFT) level, TB09 leads to band gaps in much better agreement with experiments than LDA. However, we observe that it globally underestimates, often strongly, the valence (and conduction) band widths (more than LDA). MBPT corrections are calculated starting from both LDA and TB09 eigenenergies and wavefunctions. They lead to a much better agreement with experimental data for band widths. The band gaps obtained starting from TB09 are close to those from quasi-particle self-consistent GW calculations, at a much reduced cost. Finally, we explore the possibility to tune one of the semi-empirical parameters of the TB09 functional in order to obtain simultaneously better band gaps and widths. We find that these requirements are conflicting., Comment: 18 pages, 16 figures
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- 2013
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346. Asteroseismic determination of obliquities of the exoplanet systems Kepler-50 and Kepler-65
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Chaplin, W. J., Sanchis-Ojeda, R., Campante, T. L., Handberg, R., Stello, D., Winn, J. N., Basu, S., Christensen-Dalsgaard, J., Davies, G. R., Metcalfe, T. S., Buchhave, L. A., Fischer, D. A., Bedding, T. R., Cochran, W. D., Elsworth, Y., Gilliland, R. L., Hekker, S., Huber, D., Isaacson, H., Karoff, C., Kawaler, S. D., Kjeldsen, H., Latham, D. W., Lund, M. N., Lundkvist, M., Marcy, G. W., Miglio, A., Barclay, T., and Lissauer, J. J.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
Results on the obliquity of exoplanet host stars -- the angle between the stellar spin axis and the planetary orbital axis -- provide important diagnostic information for theories describing planetary formation. Here we present the first application of asteroseismology to the problem of stellar obliquity determination in systems with transiting planets and Sun-like host stars. We consider two systems observed by the NASA Kepler Mission which have multiple transiting small (super-Earth sized) planets: the previously reported Kepler-50 and a new system, Kepler-65, whose planets we validate in this paper. Both stars show rich spectra of solar-like oscillations. From the asteroseismic analysis we find that each host has its rotation axis nearly perpendicular to the line of sight with the sines of the angles constrained at the 1-sigma level to lie above 0.97 and 0.91, respectively. We use statistical arguments to show that coplanar orbits are favoured in both systems, and that the orientations of the planetary orbits and the stellar rotation axis are correlated., Comment: Accepted for publication in ApJ; 46 pages, 11 figures
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- 2013
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347. Testing convective-core overshooting using period spacings of dipole modes in red giants
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Montalban, J., Miglio, A., Noels, A., Dupret, M. -A., Scuflaire, R., and Ventura, P.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Uncertainties on central mixing in main sequence (MS) and core He-burning (He-B) phases affect key predictions of stellar evolution such as late evolutionary phases, chemical enrichment, ages etc. We propose a test of the extension of extra-mixing in two relevant evolutionary phases based on period spacing Delta_P of solar-like oscillating giants. From stellar models and their corresponding adiabatic frequencies (respectively computed with ATON and LOSC codes) we provide the first predictions of the observable Delta_P for stars in the red giant branch (RGB) and in the red clump (RC). We find: i) a clear correlation between Delta_P and the mass of the helium core (M_He); the latter in intermediate-mass stars depends on the MS overshooting, hence it can be used to set constraints on extra mixing during MS when coupled with chemical composition; ii) a linear dependence of the average value of the asymptotic period spacing (
_a) during the He-B phase on the size of the convective core. A first comparison with the inferred asymptotic period spacing for Kepler RC stars suggests the need for extra mixing also during this phase, as evinced from other observational facts., Comment: 19 pages, 8 figures, accepted for publication in ApJ - Published
- 2013
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348. Kepler-68: Three Planets, One With a Density Between That of Earth and Ice Giants
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Gilliland, Ronald L., Marcy, Geoffrey W., Rowe, Jason F., Rogers, Leslie, Torres, Guillermo, Fressin, Francois, Lopez, Eric D., Buchhave, Lars A., Christensen-Dalsgaard, Joergen, Desert, Jean-Michel, Isaacson, Howard, Jenkins, Jon M., Lissauer, Jack L., Chaplin, William J., Basu, Sarbani, Metcalfe, Travis S., Elsworth, Yvonne, Handberg, Rasmus, Hekker, Saskia, Huber, Daniel, Karoff, Christoffer, Kjeldsen, Hans, Lund, Mikkel N., Lundkvist, Mia, Miglio, Andrea, Charbonneau, David, Ford, Eric B., Fortney, Jonathan J., Haas, Michael R., Howard, Andrew W., Howell, Steve B., Ragozzine, Darin, and Thompson, Susan E.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
NASA's Kepler Mission has revealed two transiting planets orbiting Kepler-68. Follow-up Doppler measurements have established the mass of the innermost planet and revealed a third jovian-mass planet orbiting beyond the two transiting planets. Kepler-68b, in a 5.4 day orbit has mass 8.3 +/- 2.3 Earth, radius 2.31 +/- 0.07 Earth radii, and a density of 3.32 +/- 0.92 (cgs), giving Kepler-68b a density intermediate between that of the ice giants and Earth. Kepler-68c is Earth-sized with a radius of 0.953 Earth and transits on a 9.6 day orbit; validation of Kepler-68c posed unique challenges. Kepler-68d has an orbital period of 580 +/- 15 days and minimum mass of Msin(i) = 0.947 Jupiter. Power spectra of the Kepler photometry at 1-minute cadence exhibit a rich and strong set of asteroseismic pulsation modes enabling detailed analysis of the stellar interior. Spectroscopy of the star coupled with asteroseismic modeling of the multiple pulsation modes yield precise measurements of stellar properties, notably Teff = 5793 +/- 74 K, M = 1.079 +/- 0.051 Msun, R = 1.243 +/- 0.019 Rsun, and density 0.7903 +/- 0.0054 (cgs), all measured with fractional uncertainties of only a few percent. Models of Kepler-68b suggest it is likely composed of rock and water, or has a H and He envelope to yield its density of about 3 (cgs)., Comment: 32 pages, 13 figures, Accepted to ApJ
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- 2013
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349. Fundamental Properties of Kepler Planet-Candidate Host Stars using Asteroseismology
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Huber, Daniel, Chaplin, William J., Christensen-Dalsgaard, Jørgen, Gilliland, Ronald L., Kjeldsen, Hans, Buchhave, Lars A., Fischer, Debra A., Lissauer, Jack J., Rowe, Jason F., Sanchis-Ojeda, Roberto, Basu, Sarbani, Handberg, Rasmus, Hekker, Saskia, Howard, Andrew W., Isaacson, Howard, Karoff, Christoffer, Latham, David W., Lund, Mikkel N., Lundkvist, Mia, Marcy, Geoffrey W., Miglio, Andrea, Aguirre, Victor Silva, Stello, Dennis, Arentoft, Torben, Barclay, Thomas, Bedding, Timothy R., Burke, Christopher J., Christiansen, Jessie L., Elsworth, Yvonne P., Haas, Michael R., Kawaler, Steven D., Metcalfe, Travis S., Mullally, Fergal, and Thompson, Susan E.
- Subjects
Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We have used asteroseismology to determine fundamental properties for 66 Kepler planet-candidate host stars, with typical uncertainties of 3% and 7% in radius and mass, respectively. The results include new asteroseismic solutions for four host stars with confirmed planets (Kepler-4, Kepler-14, Kepler-23 and Kepler-25) and increase the total number of Kepler host stars with asteroseismic solutions to 77. A comparison with stellar properties in the planet-candidate catalog by Batalha et al. shows that radii for subgiants and giants obtained from spectroscopic follow-up are systematically too low by up to a factor of 1.5, while the properties for unevolved stars are in good agreement. We furthermore apply asteroseismology to confirm that a large majority of cool main-sequence hosts are indeed dwarfs and not misclassified giants. Using the revised stellar properties, we recalculate the radii for 107 planet candidates in our sample, and comment on candidates for which the radii change from a previously giant-planet/brown-dwarf/stellar regime to a sub-Jupiter size, or vice versa. A comparison of stellar densities from asteroseismology with densities derived from transit models in Batalha et al. assuming circular orbits shows significant disagreement for more than half of the sample due to systematics in the modeled impact parameters, or due to planet candidates which may be in eccentric orbits. Finally, we investigate tentative correlations between host-star masses and planet candidate radii, orbital periods, and multiplicity, but caution that these results may be influenced by the small sample size and detection biases., Comment: 19 pages, 10 figures, 4 tables; accepted for publication in ApJ; machine-readable versions of tables 1-3 are available as ancillary files or in the source code; v2: minor changes to match published version
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- 2013
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350. GAUFRE: a tool for an automated determination of atmospheric parameters from spectroscopy
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Valentini, Marica, Morel, Thierry, Miglio, Andrea, Fossati, Luca, and Munari, Ulisse
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Astrophysics - Solar and Stellar Astrophysics - Abstract
We present an automated tool for measuring atmospheric parameters (T_eff, log(g), [Fe/H]) for F-G-K dwarf and giant stars. The tool, called GAUFRE, is written in C++ and composed of several routines: GAUFRE-RV measures radial velocity from spectra via cross-correlation against a synthetic template, GAUFRE-EW measures atmospheric parameters through the classic line-by-line technique and GAUFRE-CHI2 performs a chi^2 fitting to a library of synthetic spectra. A set of F-G-K stars extensively studied in the literature were used as a benchmark for the program: their high signal-to-noise and high resolution spectra were analysed by using GAUFRE and results were compared with those present in literature. The tool is also implemented in order to perform the spectral analysis after fixing the surface gravity (log(g)) to the accurate value provided by asteroseismology. A set of CoRoT stars, belonging to LRc01 and LRa01 fields was used for first testing the performances and the behaviour of the program when using the seismic log(g)., Comment: 7 pages, 3 figures, to appear in proceedings of 40th Liege International Astrophysical Colloquium 'Ageing low-mass stars: from red giants to white dwarfs'
- Published
- 2013
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