20 results on '"D. Pricopi"'
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2. PLATO as it is: A legacy mission for Galactic archaeology
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A. Miglio, C. Chiappini, B. Mosser, G. R. Davies, K. Freeman, L. Girardi, P. Jofré, D. Kawata, B. M. Rendle, M. Valentini, L. Casagrande, W. J. Chaplin, G. Gilmore, K. Hawkins, B. Holl, T. Appourchaux, K. Belkacem, D. Bossini, K. Brogaard, M.‐J. Goupil, J. Montalbán, A. Noels, F. Anders, T. Rodrigues, G. Piotto, D. Pollacco, H. Rauer, C. Allende Prieto, P. P. Avelino, C. Babusiaux, C. Barban, B. Barbuy, S. Basu, F. Baudin, O. Benomar, O. Bienaymé, J. Binney, J. Bland‐Hawthorn, A. Bressan, C. Cacciari, T. L. Campante, S. Cassisi, J. Christensen‐Dalsgaard, F. Combes, O. Creevey, M. S. Cunha, R. S. Jong, P. Laverny, S. Degl'Innocenti, S. Deheuvels, É. Depagne, J. Ridder, P. Di Matteo, M. P. Di Mauro, M.‐A. Dupret, P. Eggenberger, Y. Elsworth, B. Famaey, S. Feltzing, R. A. García, O. Gerhard, B. K. Gibson, L. Gizon, M. Haywood, R. Handberg, U. Heiter, S. Hekker, D. Huber, R. Ibata, D. Katz, S. D. Kawaler, H. Kjeldsen, D. W. Kurtz, N. Lagarde, Y. Lebreton, M. N. Lund, S. R. Majewski, P. Marigo, M. Martig, S. Mathur, I. Minchev, T. Morel, S. Ortolani, M. H. Pinsonneault, B. Plez, P. G. Prada Moroni, D. Pricopi, A. Recio‐Blanco, C. Reylé, A. Robin, I. W. Roxburgh, M. Salaris, B. X. Santiago, R. Schiavon, A. Serenelli, S. Sharma, V. Silva Aguirre, C. Soubiran, M. Steinmetz, D. Stello, K. G. Strassmeier, P. Ventura, R. Ventura, N. A. Walton, and C. C. Worley
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- 2017
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3. A radiation transfer model for the Milky Way. II The global properties and large scale structure
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Cristina C. Popescu, M. T. Rushton, Giovanni Natale, D. Pricopi, Ruizhi Yang, and Jordan J. Thirlwall
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Physics ,Spiral galaxy ,Stellar mass ,Star formation ,Milky Way ,Astrophysics::High Energy Astrophysical Phenomena ,Extinction (astronomy) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Solar radius ,F500 ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Thin disk ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
We obtained an axi-symmetric model for the large-scale distribution of stars and dust in the Milky Way (MW) using a radiative transfer code that can account for the existing near-infrared (NIR)/mid-infrared/submm all-sky emission maps of our Galaxy. We find that the MW has a star-formation rate of ${ SFR}=1.25\pm0.2\,{ M}_{\odot}$/yr, a stellar mass $M_{*}=(4.9\pm 0.3)\times10^{10}\,{ M}_{\odot}$, and a specific SFR that is relatively constant with radius (except for the inner 1 kpc). We identified an inner radius $R_{ in}= 4.5$\,kpc beyond which the stellar emissivity and dust distribution fall exponentially. For $R, Comment: Accepted for publication in MNRAS, 25 pages, 21 figures
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- 2021
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4. Orbits stability under the influence of Mücket-Treder potential
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D. Pricopi and E. Popescu
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Physics ,Angular momentum ,Field (physics) ,Structure (category theory) ,Equations of motion ,Astronomy and Astrophysics ,01 natural sciences ,Stability (probability) ,Cosmology ,Classical mechanics ,Space and Planetary Science ,0103 physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,Polar coordinate system ,Constant (mathematics) ,010303 astronomy & astrophysics - Abstract
The Mucket-Treder-type potential was initially introduced to explain the discrepancy between Mercury’s observed perihelion advance and the computed value based on Newton’s law, but it can also be used for many astronomical situations as, for instance, the study of the very eccentric cometary orbits in the neighborhood of the Sun. In this paper we tackle the two-body problem in the Mucket-Treder post-Newtonian field from the particular standpoint of orbits stability. Starting from the equations of motion and first integrals written in standard polar coordinates, we apply McGehee-type transformations of the second kind. Then we depict the phase-space structure considering the foliations by the energy constant and the angular momentum constant. Various stability regions are found for each case.
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- 2020
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5. Global flow in the generalized Buckingham’s two-body problem
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E. Popescu and D. Pricopi
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Physics ,Buckingham ,Angular momentum ,Phase portrait ,010102 general mathematics ,Mathematical analysis ,Zero (complex analysis) ,Astronomy and Astrophysics ,Two-body problem ,01 natural sciences ,Classical mechanics ,Space and Planetary Science ,0103 physical sciences ,0101 mathematics ,Variety (universal algebra) ,Constant (mathematics) ,010303 astronomy & astrophysics ,Buckingham potential - Abstract
In this paper, we consider the generalized Buckingham potential. Using the McGehee’s regularizing transformations, we study the global flow for the two-body problem associated to this potential. By making vary the angular momentum constant in the three cases of negative, zero, and positive energy, we analyze all possible situations. In each case, we obtain the global flow of the problem, exhibiting a great variety of orbits. All phase portraits are interpreted in terms of physical trajectories.
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- 2017
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6. Stability of the celestial body orbits under the influence of Yukawa potential
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D. Pricopi
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Physics ,Angular momentum ,Lebesgue measure ,010308 nuclear & particles physics ,Yukawa potential ,Equations of motion ,Classical field theory ,Astronomy and Astrophysics ,01 natural sciences ,Celestial mechanics ,Classical mechanics ,Space and Planetary Science ,0103 physical sciences ,Angular momentum coupling ,Constant (mathematics) ,010303 astronomy & astrophysics - Abstract
The famous Yukawa-type potential was very often used for explaining a great variety of recent observed astronomical phenomena which range from the solar-system scale to cosmological distances. In this paper we tackle the two-body problem in the Yukawa post-Newtonian field from the particular standpoint of orbits stability. Starting from the equations of motion and first integrals written in standard polar coordinates, we apply McGehee-type transformations of the second kind. Then we depict the phase-space structure considering the foliations by the energy constant and the angular momentum constant. Various stability regions are found for each case. The problem presents interesting features, such as: cases when all trajectories (maybe except for a separatrix) are stable; cases when there exist totally different types of orbits, both stable and unstable, for the same values of the energy constant and the angular momentum constant; the existence of stable motion for nonnegative energy levels; positive Lebesgue measure for initial data leading to quasiperiodic and noncircular periodic orbits; the key role of the angular momentum.
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- 2016
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7. Phase-space structure of the Buckingham’s two-body problem
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E. Popescu and D. Pricopi
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Physics ,Angular momentum ,010304 chemical physics ,Phase portrait ,Equations of motion ,Motion (geometry) ,Astronomy and Astrophysics ,Phase plane ,Two-body problem ,01 natural sciences ,Classical mechanics ,Space and Planetary Science ,Phase space ,0103 physical sciences ,010303 astronomy & astrophysics ,Buckingham potential - Abstract
In this paper, we study the global flow for the two-body problem associated to the Buckingham potential. For this, using McGehee-type transformations, we write the regularized equations of motion. Then, reducing the 4-dimensional phase space to a 2-dimension one, the global flow in the phase plane is described for all possible values of the parameters of the potential and those of the energy and angular momentum constants. Every phase trajectory is interpreted in terms of physical motion, our problem being depicted both geometrically and physically.
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- 2016
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8. Kepler observations of the high-amplitude δ Scuti star V2367 Cyg
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Joanna Molenda-Żakowicz, S. Bernabei, L. A. Balona, Vincenzo Ripepi, A. Moya, D. Pricopi, Todd C. Klaus, Jadwiga Daszyńska-Daszkiewicz, Marcella Marconi, Giovanni Catanzaro, Victoria Antoci, Karen Kinemuchi, A. Grigahcène, M. Di Criscienzo, J. C. Suárez, M. D. Suran, Patrick Lenz, Barry Smalley, Andrzej Pigulski, Gerald Handler, D. W. Kurtz, J. M. Nemec, and Jennifer R. Hall
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Physics ,Mode (statistics) ,Astronomy and Astrophysics ,Angular velocity ,Astrophysics ,Star (graph theory) ,Kepler ,Stars ,Amplitude ,Space and Planetary Science ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Variation (astronomy) ,Order of magnitude - Abstract
We analyse Kepler observations of the high-amplitude δ Scuti (HADS) star V2367 Cyg (KIC 9408694). The variations are dominated by a mode with frequency f1= 5.6611 d−1. Two other independent modes with f2= 7.1490 d−1 and f3= 7.7756 d−1 have amplitudes an order of magnitude smaller than f1. Nearly all the light variation is due to these three modes and their combination frequencies, but several hundred other frequencies of very low amplitude are also present. The amplitudes of the principal modes may vary slightly with time. The star has twice the projected rotational velocity of any other HADS star, which makes it unusual. We find a correlation between the phases of the combination frequencies and their pulsation frequencies, which is not understood. Since modes of highest amplitude in HADS stars are normally radial modes, we assumed that this would also be true in this star. However, attempts to model the observed frequencies as radial modes without mode interaction were not successful. For a star with such a relatively high rotational velocity, it is important to consider the effect of mode interaction. Indeed, when this was done, we were able to obtain a model in which a good match with f1 and f2 is obtained, with f1 being the fundamental radial mode.
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- 2011
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9. Kepler observations of the variability in B-type stars
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L. A. Balona, A. Pigulski, P. De Cat, G. Handler, J. Gutiérrez-Soto, C. A. Engelbrecht, F. Frescura, M. Briquet, J. Cuypers, J. Daszyńska-Daszkiewicz, P. Degroote, R. J. Dukes, R. A. Garcia, E. M. Green, U. Heber, S. D. Kawaler, H. Lehmann, B. Leroy, J. Molenda-Żakowicz, C. Neiner, A. Noels, J. Nuspl, R. Østensen, D. Pricopi, I. Roxburgh, S. Salmon, M. A. Smith, J. C. Suárez, M. Suran, R. Szabó, K. Uytterhoeven, null Christensen-Dalsgaard, H. Kjeldsen, D. A. Caldwell, F. R. Girouard, and D. T. Sanderfer
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Physics ,Binary number ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Type (model theory) ,Rotation ,Light curve ,Instability ,Spectral line ,Stars ,Space and Planetary Science ,Modulation (music) ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
The analysis of the light curves of 48 B-type stars observed by Kepler is presented. Among these are 15 pulsating stars, all of which show low frequencies characteristic of SPB stars. Seven of these stars also show a few weak, isolated high frequencies and they could be considered as SPB/beta Cep hybrids. In all cases the frequency spectra are quite different from what is seen from ground-based observations. We suggest that this is because most of the low frequencies are modes of high degree which are predicted to be unstable in models of mid-B stars. We find that there are non-pulsating stars within the beta Cep and SPB instability strips. Apart from the pulsating stars, we can identify stars with frequency groupings similar to what is seen in Be stars but which are not Be stars. The origin of the groupings is not clear, but may be related to rotation. We find periodic variations in other stars which we attribute to proximity effects in binary systems or possibly rotational modulation. We find no evidence for pulsating stars between the cool edge of the SPB and the hot edge of the delta Sct instability strips. None of the stars show the broad features which can be attributed to stochastically-excited modes as recently proposed. Among our sample of B stars are two chemically peculiar stars, one of which is a HgMn star showing rotational modulation in the light curve.
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- 2011
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10. Asteroseismic modeling of the pulsating B star HD163830
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D. Pricopi and M. D. Suran
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Physics ,Gravity (chemistry) ,Oscillation ,Astrophysics ,Star (graph theory) - Abstract
In this paper, we report our preliminary results regarding the asteroseismic modeling of the slow pulsating B star HD 163830, based on eighteen of the twenty detected frequencies of this star. The powerful method of matching stellar models both to oscillation data and eective temperature and gravity of HD 163830 is applied to identify a best-t model. These eighteen frequencies correspond to low-order, high-degree g-modes of an stellar model of 1:016 10 8 yr, of a 4:4M star with chemical composition X = 0:71, Z = 0:02.
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- 2008
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11. Luminosity variation in the extended one-zone RR Lyrae model
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D. Pricopi
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Physics ,stars: variables: RR Lyr ,lcsh:Astronomy ,Shell (structure) ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,RR Lyrae variable ,stars: interiors ,Light curve ,Ideal gas ,Luminosity ,lcsh:QB1-991 ,Nonlinear system ,Stars ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Stellar pulsation ,Astrophysics::Galaxy Astrophysics - Abstract
The Stellingwerf one-zone stellar model is extended by assuming, a slow and uniform rotation that leads to a very small oblateness of the star. The matter in the core-surrounding shell is supposed to consists of a mixture of ideal gas and radiation. This one-zone stellar pulsation model is proposed as a tool to investigate the factors affecting luminosity variations of pulsating stars. Linear and nonlinear analyses of the resulting equations are described. The results are in very good agreement with the observed RR Lyrae light curves. .
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- 2005
12. Properties of 42 Solar-type Kepler Targets from the Asteroseismic Modeling Portal
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M. Di Mauro, Timothy R. White, M. Steslicki, Margarida S. Cunha, Karan Molaverdikhani, T. S. Metcalfe, A. M. Serenelli, Benjamin P. Brown, R. Trampedach, Dennis Stello, William J. Chaplin, Sébastien Deheuvels, Derek Buzasi, R. Simoniello, Anwesh Mazumdar, Guy R. Davies, Timothy R. Bedding, Mário J. P. F. G. Monteiro, Jørgen Christensen-Dalsgaard, Rachel Howe, Mutlu Yildiz, O. L. Creevey, Yvonne Elsworth, David B. Guenther, K. B. MacGregor, Othman Benomar, S. Mathur, Yveline Lebreton, Aliz Derekas, Rafael A. García, Christoffer Karoff, G. Doğan, Haiying Xu, D. Pricopi, Tiago L. Campante, D. Salabert, Josefina Montalbán, Z. Celik, M. D. Suran, M. Gruberbauer, C. Aksoy, J. A. Guzik, High Altitude Observatory (HAO), National Center for Atmospheric Research [Boulder] (NCAR), Computational and Information Systems Laboratory (CISL), Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Torino (UNITO), Dept. Electrical and Computer Engineering, University of Minnesota, University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, BIT lab (BIT Lab), Université Galatasaray (GSU), Department of Astronomy and Physics [Halifax], Saint Mary's University [Halifax], Inorgan Chem Lab, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Ege Üniversitesi, Università degli studi di Torino = University of Turin (UNITO), and Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)
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oscillations [stars] ,FOS: Physical sciences ,Astrophysics ,Type (model theory) ,stars: interiors ,01 natural sciences ,Kepler ,methods: numerical ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,stars: evolution ,010303 astronomy & astrophysics ,Scaling ,Solar and Stellar Astrophysics (astro-ph.SR) ,ComputingMilieux_MISCELLANEOUS ,Physics ,interiors [stars] ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,Oscillation ,Subgiant ,Mode (statistics) ,Astronomy and Astrophysics ,numerical [methods] ,Radius ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,evolution [stars] ,Astrophysics::Earth and Planetary Astrophysics ,stars: oscillations - Abstract
WOS: 000344141500013, Recently the number of main-sequence and subgiant stars exhibiting solar-like oscillations that are resolved into individual mode frequencies has increased dramatically. While only a few such data sets were available for detailed modeling just a decade ago, the Kepler mission has produced suitable observations for hundreds of new targets. This rapid expansion in observational capacity has been accompanied by a shift in analysis and modeling strategies to yield uniform sets of derived stellar properties more quickly and easily. We use previously published asteroseismic and spectroscopic data sets to provide a uniform analysis of 42 solar-type Kepler targets from the Asteroseismic Modeling Portal. We find that fitting the individual frequencies typically doubles the precision of the asteroseismic radius, mass, and age compared to grid-based modeling of the global oscillation properties, and improves the precision of the radius and mass by about a factor of three over empirical scaling relations. We demonstrate the utility of the derived properties with several applications., NASANational Aeronautics & Space Administration (NASA) [NNX13AC44G, NNX13AE91G]; White Dwarf Research Corporation through the Pale Blue Dot project; Danish National Research FoundationDanmarks Grundforskningsfond [DNRF106]; European Research CouncilEuropean Research Council (ERC) [267864]; Scientific and Technological Research Council of TurkeyTurkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK) [TUBITAK:112T989]; European Commission grant for the SPACEINN project [FP7-SPACE-2012-312844]; NSF Astronomy and Astrophysics postdoctoral fellowshipNational Science Foundation (NSF) [AST 09-02004]; NSFNational Science Foundation (NSF) [PHY 08-21899, PHY 11-25915]; Investigador FCT contract - FCT/MCTES (Portugal); POPH/FSE (EC)European Commission Joint Research CentreEuropean Social Fund (ESF); Hungarian OTKAOrszagos Tudomanyos Kutatasi Alapprogramok (OTKA) [K83790, KTIA URKUT_10-1-2011-0019]; Lendulet Young Researchers Programme of the Hungarian Academy of Sciences; Janos Bolyai Research Scholarship of the Hungarian Academy of SciencesHungarian Academy of Sciences; City of Szombathely [S-11-1027]; European Community Seventh Framework Programme (FP7) [269194 (IRSES/ASK)]; CNES grant at CEA-Saclay; NIUS programme of HBCSE (TIFR); MICINN grant [AYA2011-24704]; ESF EUROCORES Program EuroGENESIS (MICINN) [EUI2009-04170]; Australian Research CouncilAustralian Research Council; Science and Technology Facilities CouncilScience & Technology Facilities Council (STFC) [ST/J001163/1], We would like to thank Victor Silva Aguirre for helpful discussions. This work was supported in part by NASA grants NNX13AC44G and NNX13AE91G, and by White Dwarf Research Corporation through the Pale Blue Dot project (http://whitedwarf.org/palebluedot/). Computational time on Kraken at the National Institute of Computational Sciences was provided through XSEDE allocation TG-AST090107. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant DNRF106). We acknowledge the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No.: 267864), the Scientific and Technological Research Council of Turkey (TUBITAK:112T989), and a European Commission grant for the SPACEINN project (FP7-SPACE-2012-312844). B.P.B. was supported in part by NSF Astronomy and Astrophysics postdoctoral fellowship AST 09-02004. C.M.S.O. is supported by NSF grant PHY 08-21899 and K.I.T.P. is supported by NSF grant PHY 11-25915. M.S.C. is supported by an Investigador FCT contract funded by FCT/MCTES (Portugal) and POPH/FSE (EC). A.D. has been supported by the Hungarian OTKA grants K83790, KTIA URKUT_10-1-2011-0019 grant, the Lendulet-2009 Young Researchers Programme of the Hungarian Academy of Sciences, the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences and the City of Szombathely under agreement No. S-11-1027. A.D. and R.A.G. acknowledge the support of the European Community Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 269194 (IRSES/ASK). R.A.G. and D. Salabert acknowledge the support of the CNES grant at CEA-Saclay. A.M. acknowledges support from the NIUS programme of HBCSE (TIFR). A.S. is supported by the MICINN grant AYA2011-24704 and by the ESF EUROCORES Program EuroGENESIS (MICINN grant EUI2009-04170). D. Stello is supported by the Australian Research Council.
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- 2014
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13. Evidence for a source of H chondrites in the outer main asteroid belt
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Dan Alin Nedelcu, D. Pricopi, Marcel Popescu, Octavian Badescu, Mirel Birlan, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
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Physics ,[PHYS]Physics [physics] ,Potentially hazardous object ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Parent body ,Jupiter ,Meteorite ,13. Climate action ,Space and Planetary Science ,Chondrite ,Asteroid ,[SDU]Sciences of the Universe [physics] ,Asteroid belt ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,ComputingMilieux_MISCELLANEOUS ,Ordinary chondrite - Abstract
Aims. In this paper we report near-infrared spectroscopic observations of one of the largest potentially hazardous asteroids, (214869) 2007 PA8. Mineralogical analysis of this object was followed by the investigation of the dynamical delivery mechanism from its probable source region, based on long-term numerical integrations. Methods. The spectrum of (214869) 2007 PA8 was analysed using the positions of 1 μ ma nd 2μm bands and by curve-matching with RELAB meteorites spectra. Its dynamical evolution was investigated by means of a 200 000-year numerical integration in the past of 1275 clones followed to the source region. Results. (214869) 2007 PA8 has a very young surface with a composition more akin to H chondrites than to any other type of ordinary chondrite. It arrived from the outer Main Belt in the near-Earth space via the 5:2 mean motion resonance with Jupiter by eccentricity pumping. Identification of its source region far from (6) Hebe raises the possibility of the existence of a second parent body of the H chondrites that has a radically different post-accretion history. Future spectroscopic surveys in the 5:2 resonance region will most likely discover other asteroids with an H chondrite composition.
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- 2014
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14. ASTEROSEISMIC FUNDAMENTAL PROPERTIES OF SOLAR-TYPE STARS OBSERVED BY THE NASA KEPLER MISSION
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Andrea Miglio, Travis S. Metcalfe, Savita Mathur, Aldo Serenelli, D. Pricopi, Christoffer Karoff, Enrico Corsaro, William J. Chaplin, Clara Régulo, B. Mosser, V. Silva Aguirre, Patrick Gaulme, Saskia Hekker, Tiago L. Campante, Alfio Bonanno, O. L. Creevey, Jørgen Christensen-Dalsgaard, Rafael A. García, M. D. Suran, D. Salabert, Dennis Stello, Sarbani Basu, G. Houdek, J. P. Marques, J. Molenda-Zakowicz, Warrick H. Ball, Mário J. P. F. G. Monteiro, Laurent Gizon, Rasmus Handberg, T. Appourchaux, R. Lutz, Hans Kjeldsen, Yvonne Elsworth, Luca Casagrande, Daniel Huber, NOAA Earth System Research Laboratory (ESRL), National Oceanic and Atmospheric Administration (NOAA), Service d’orthopédie et traumatologie pédiatrique [CHRU Nancy], Centre Hospitalier Régional Universitaire de Nancy (CHRU Nancy), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), Kavli Institute for Theoretical Physics [Santa Barbara] (KITP), University of California [Santa Barbara] (UC Santa Barbara), University of California (UC)-University of California (UC), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Aarhus], Aarhus University [Aarhus], School of Physics and Astronomy [Birmingham], University of Birmingham [Birmingham], Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, School of Physics [UNSW Sydney] (UNSW), University of New South Wales [Sydney] (UNSW), Astronomical Institute [Wroclaw], University of Wrocław [Poland] (UWr), Stellar Astrophysics Centre [Aarhus] (SAC), School of Physics and Astronomy, Institut de Physique du Globe de Paris (IPG Paris), Institute for Astronomy [Vienna], University of Vienna [Vienna], INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), Space Science Institute [Boulder] (SSI), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), University of California [Santa Barbara] (UCSB), University of California-University of California, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris, and Low Energy Astrophysics (API, FNWI)
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fundamental parameters [stars] ,FOS: Physical sciences ,asteroseismology ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Type (model theory) ,01 natural sciences ,7. Clean energy ,Kepler ,Photometry (optics) ,0103 physical sciences ,data analysis [methods] ,Astrophysics::Solar and Stellar Astrophysics ,Gyrochronology ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,ComputingMilieux_MISCELLANEOUS ,interiors [stars] ,Physics ,[PHYS]Physics [physics] ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Homogeneous ,Astrophysics::Earth and Planetary Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - 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)
- Published
- 2014
- Full Text
- View/download PDF
15. Ensemble asteroseismology of solar-type stars with the NASA Kepler mission
- Author
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Mário J. P. F. G. Monteiro, Tiago L. Campante, L. Esch, William J. Borucki, M. D. Suran, Dennis Stello, Graham A. Verner, Travis S. Metcalfe, Jon M. Jenkins, Jørgen Christensen-Dalsgaard, Alfio Bonanno, Enrico Corsaro, William J. Chaplin, Andrea Miglio, D. Salabert, Savita Mathur, Orlagh Creevey, J. Van Cleve, Joanna Molenda-Żakowicz, I. M. Brandão, Daniel Huber, Steven J. Hale, Christoffer Karoff, Jérôme Ballot, G. Houdek, D. Pricopi, Aldo Serenelli, Rafael A. García, L. Girardi, Todd C. Klaus, Yvonne Elsworth, H. Bruntt, Patrick Gaulme, S. G. Sousa, Saskia Hekker, A.-M. Broomhall, Timothy R. Bedding, Roger New, P.-O. Quirion, Ian R. Stevens, Ning Gai, T. Appourchaux, Ronald L. Gilliland, V. Silva Aguirre, Michael Thompson, Sarbani Basu, Timothy R. White, S. D. Kawaler, Clara Régulo, Marc H. Pinsonneault, G. Doğan, K. Uytterhoeven, Timothy M. Brown, Anwesh Mazumdar, Hans Kjeldsen, Karen Kinemuchi, Rasmus Handberg, B. Mosser, Antonio Jiménez, School of Physics and Astronomy, University of Birmingham [Birmingham], Aarhus University [Aarhus], Yale University [New Haven], Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Sydney Institute for Astronomy (SIfA), The University of Sydney, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Space Telescope Science Institute (STSci), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), University of Vienna [Vienna], Iowa State University (ISU), High Altitude Observatory (HAO), National Center for Atmospheric Research [Boulder] (NCAR), University of Wrocław [Poland] (UWr), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Catania (OACT), Universidad de La Laguna [Tenerife - SP] (ULL), Instituto de Astrofisica de Canarias (IAC), Homi Bhabha National Institute (HBNI), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Materials and Engineering Research Institute [Sheffield] (MERI), Sheffield Hallam University, Ohio State University [Columbus] (OSU), Astronomical Institute of Romanian Academy, Romanian Academy, Canadian Space Agency (CSA), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Max Planck Institute for Astrophysics, Max-Planck-Gesellschaft, NASA Ames Research Center (ARC), Las Cumbres Observatory (LCO), Low Energy Astrophysics (API, FNWI), Stellar Astrophysics Centre [Aarhus] (SAC), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universidade do Porto, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Faculdade de Ciências
- Subjects
Astronomia, Física ,Física [Ciências exactas e naturais] ,010504 meteorology & atmospheric sciences ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Asteroseismology ,Kepler Input Catalog ,Kepler-47 ,Physical sciences [Natural sciences] ,Astronomy, Physical sciences ,Stellar dynamics ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Kepler-62 ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Physics ,Multidisciplinary ,[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR] ,Stellar collision ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Exoplanet ,Astrophysics - Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Kepler-62c - Abstract
In addition to its search for extra-solar planets, the NASA Kepler Mission provides exquisite data on stellar oscillations. We report the detections of oscillations in 500 solartype stars in the Kepler field of view, an ensemble that is large enough to allow statistical studies of intrinsic stellar properties (such as mass, radius and age) and to test theories of stellar evolution. We find that the distribution of observed masses of these stars shows intriguing differences to predictions from models of synthetic stellar populations in the Galaxy., 20 pages, including on-line supporting material
- Published
- 2011
- Full Text
- View/download PDF
16. Predicting the detectability of oscillations in solar-type stars observed by Kepler
- Author
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T. Appourchaux, Mário J. P. F. G. Monteiro, R. L. Gilliland, Tiago L. Campante, David G. Koch, Jørgen Christensen-Dalsgaard, J. M. Jenkins, Clara Régulo, A.-M. Broomhall, Marc H. Pinsonneault, B. Mosser, Michael Thompson, D. Pricopi, Alfio Bonanno, T. S. Metcalfe, Christoffer Karoff, Jessie L. Christiansen, B. D. Clarke, Hans Kjeldsen, Todd C. Klaus, William J. Borucki, Rasmus Handberg, Steven D. Kawaler, Graham A. Verner, L. Esch, D. Salabert, Timothy M. Brown, Sarbani Basu, Ning Gai, Timothy R. Bedding, O. L. Creevey, G. Houdek, Patrick Gaulme, Saskia Hekker, S. T. Bryson, Dennis Stello, Roger New, P.-O. Quirion, Yvonne Elsworth, J. Molenda-Zakowicz, Natalie M. Batalha, Daniel Huber, Savita Mathur, Enrico Corsaro, William J. Chaplin, Jérôme Ballot, Steven J. Hale, Rafael A. García, M. D. Suran, Deokkeun An, O. Benomar, Ian W. Roxburgh, School of Physics and Astronomy, University of Birmingham, Danish AsteroSeismology Centre (DASC), Sydney Institute for Astronomy (SIfA), Space Telescope Science Institute (STScI), Department of Physics and Astronomy, Iowa State University, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut für Astronomie, Universität Wien (IfA), High Altitude Observatory, National Center for Atmospheric Research, Astronomical Institute, University of Wroclaw, Centro de Astrofísica, Universidade do Porto, National Aeronautics and Space Administration, Ames Research Center, Las Cumbres Observatory, Goleta, SETI Institute, NASA Ames Research Center, Moffett Field, Orbital Sciences Corporation, NASA Ames Research Center, Moffett Field, Department of Science Education, Ewha Womans University, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Department of Astronomy, Yale University, INAF-Osservatorio Astrofisico di Catania (INAF-OACt), Universidad de La Laguna [Tenerife - SP] (ULL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Etoile, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Materials Engineering Research Institute, Faculty of Arts, Computing, Engineering and Sciences, Sheffield Hallam University, Department of Astronomy, Ohio State University, Astronomical Institute of the Romanian Academy, Bucharest, Canadian Space Agency (CSA), Instituto de Astrofísica de Canarias (IAC), Astronomy Unit, Queen Mary, and Low Energy Astrophysics (API, FNWI)
- Subjects
Physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Radius ,Type (model theory) ,Kepler ,Asteroseismology ,Exoplanet ,Stars ,Apparent magnitude ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Physics::Space Physics ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
Asteroseismology of solar-type stars has an important part to play in the exoplanet program of the NASA Kepler Mission. Precise and accurate inferences on the stellar properties that are made possible by the seismic data allow very tight constraints to be placed on the exoplanetary systems. Here, we outline how to make an estimate of the detectability of solar-like oscillations in any given Kepler target, using rough estimates of the temperature and radius, and the Kepler apparent magnitude., Comment: 21 pages, 6 figures, accepted for publication Astrophysical Journal
- Published
- 2011
- Full Text
- View/download PDF
17. Pulsational Stability of Red Giant Stars
- Author
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D. Pricopi, M. D. Suran, Joyce Ann Guzik, and Paul A. Bradley
- Subjects
Physics ,Convection ,Red giant ,Astrophysics::High Energy Astrophysical Phenomena ,Numerical analysis ,Stellar atmosphere ,Astronomy ,Perturbation (astronomy) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Giant star ,Stars ,Radiative transfer ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
We revisit the problem of pulsational stability of radial and strongly trapped non‐radial modes of red giant stars. We present the results of numerical computations of oscillation properties of a 2.03 M⊙ evolutionary stellar model along the AGB. We examine the pulsational stability by taking into account the effect of perturbation of convective flux during the pulsation. Results obtained by using the standard “frozen” convection are presented for comparison.
- Published
- 2009
- Full Text
- View/download PDF
18. Astreroseismological results for the star V351 Ori
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M. D. Suran and D. Pricopi
- Subjects
Physics ,Common point ,Position (vector) ,Astrophysics::Solar and Stellar Astrophysics ,Inverse transform sampling ,Astronomy ,Astrophysics ,Star (graph theory) ,Stability (probability) ,Astrophysics::Galaxy Astrophysics - Abstract
In this paper we present the results obtained for the star V351 Ori using CESAM evolutive model combined with the ROMOSC inversion method. The inversion method is based on a (O − C)2 minimum search for the observed modes combined with the nonadiabatic stability condition of the mode and assuming the range for Te given by observations.The HR position obtained for the star is in the vicinity of the pms/postms common point, which lies far from the main sequence. A discussion about the evolutive status of the star (pms/postms) is also made.
- Published
- 2007
- Full Text
- View/download PDF
19. Solar-like stars seismology
- Author
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M. D. Suran and D. Pricopi
- Subjects
Physics ,Stars ,Space and Planetary Science ,Inverse transform sampling ,Spectral density ,Astronomy and Astrophysics ,Astrophysics - Abstract
Many solar like stars were observed by CoRoT and MOST missions. We try to investigate some of these stars using asteroseismic inversion method using both frequencies fitting and separation fitting. Our results are compared with semiempirical method based on direct power spectrum analysis.
- Published
- 2009
- Full Text
- View/download PDF
20. Ensemble asteroseismology of solar-type stars with the NASA Kepler mission.
- Author
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Chaplin WJ, Kjeldsen H, Christensen-Dalsgaard J, Basu S, Miglio A, Appourchaux T, Bedding TR, Elsworth Y, García RA, Gilliland RL, Girardi L, Houdek G, Karoff C, Kawaler SD, Metcalfe TS, Molenda-Żakowicz J, Monteiro MJ, Thompson MJ, Verner GA, Ballot J, Bonanno A, Brandão IM, Broomhall AM, Bruntt H, Campante TL, Corsaro E, Creevey OL, Doğan G, Esch L, Gai N, Gaulme P, Hale SJ, Handberg R, Hekker S, Huber D, Jiménez A, Mathur S, Mazumdar A, Mosser B, New R, Pinsonneault MH, Pricopi D, Quirion PO, Régulo C, Salabert D, Serenelli AM, Silva Aguirre V, Sousa SG, Stello D, Stevens IR, Suran MD, Uytterhoeven K, White TR, Borucki WJ, Brown TM, Jenkins JM, Kinemuchi K, Van Cleve J, and Klaus TC
- Abstract
In addition to its search for extrasolar planets, the NASA Kepler mission provides exquisite data on stellar oscillations. We report the detections of oscillations in 500 solar-type stars in the Kepler field of view, an ensemble that is large enough to allow statistical studies of intrinsic stellar properties (such as mass, radius, and age) and to test theories of stellar evolution. We find that the distribution of observed masses of these stars shows intriguing differences to predictions from models of synthetic stellar populations in the Galaxy.
- Published
- 2011
- Full Text
- View/download PDF
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