7 results on '"Lissauer, J.J."'
Search Results
2. TESS discovery of a super-earth and three sub-neptunes hosted by the bright, sunlike star HD 108236
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Henze, C.E., Bouma, L.G., Badenas-Agusti, M., Seager, S., Ziegler, C., Collins, K.A., Crane, J.D., Vanderspek, R., Law, N., Kielkopf, J.F., Kristiansen, M.H., Guerra, P., Butler, R.P., Anderson, D.R., Huang, C.X., Collins, K.I., Howell, S.B., Hellier, C., Ricker, G.R., Fulton, B., Jenkins, J.M., Ciardi, D.R., Shporer, A., Rackham, B.V., Quintana, E., Jontof, D., Scott, N., Soubkiou, A., Charbonneau, D., Winn, J.N., Briceño, C., Schwarz, R.P., Massey, B., Terentev, I.A., Kane, S.R., Rodriguez, J.E., Pinglé, K., Ting, E.B., Wright, J., Mikal-Evans, T., Shectman, S.A., Cloutier, R., Furesz, G., Berta-Thompson, Z.K., Furlan, E., Zouhair, B., Daylan, T., Lissauer, J.J., Quinn, S.N., Teske, J.K., Fong, W., Matson, R., Stassun, K.G., Vanderburg, A., Bastürk, Ö., Morgan, E.H., Schwengeler, H.M., Mann, A.W., Jensen, E.L.N., Twicken, J.D., Günther, M.N., and Irwin, J.M.
- Abstract
We report the discovery and validation of four extrasolar planets hosted by the nearby, bright, Sun-like (G3V) star HD 108236 using data from the Transiting Exoplanet Survey Satellite (TESS). We present transit photometry, reconnaissance, and precise Doppler spectroscopy, as well as high-resolution imaging, to validate the planetary nature of the objects transiting HD 108236, also known as the TESS Object of Interest (TOI) 1233. The innermost planet is a possibly rocky super-Earth with a period of 3.79523+0.00047-0.00044 days and has a radius of 1.586 ± 0.098 R⊗.The outer planets are sub-Neptunes, with potential gaseous envelopes, having radii of 2.068+0.10-0.091 R⊗, 2.72 ± 0.11 R⊗, and 3.12+0.13-0.12 R⊗ and periods of 6.20370+0.00064-0.00052 days, 14.17555+0.00099-0.0011 days, and 19.5917+0.0022-0.0020 days, respectively. With V and Ks magnitudes of 9.2 and 7.6, respectively, the bright host star makes the transiting planets favorable targets for mass measurements and, potentially, for atmospheric characterization via transmission spectroscopy. HD 108236 is the brightest Sun-like star in the visual (V ) band known to host four or more transiting exoplanets. The discovered planets span a broad range of planetary radii and equilibrium temperatures and share a common history of insolation from a Sun-like star (R∗ = 0.888 ± 0.017 R⊙, Teff = 5730 ± 50 K), making HD 108236 an exciting, opportune cosmic laboratory for testing models of planet formation and evolution.
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- 2021
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3. The CARMENES search for exoplanets around M dwarfs: Two planets on opposite sides of the radius gap transiting the nearby M dwarf LTT 3780
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Parviainen, H., Molaverdikhani, K., Jeffers, S.V., Diéz Alonso, E., Trifonov, T., Rodríguez-López, C., Caballero, J.A., Schlecker, M., Esparza-Borges, E., Montes, D., Lodieu, N., Nagel, E., Massey, B., Vanderspek, R., Stangret, M., Tanner, A., Guerra, P., Cale, B., Zapatero Osorio, M.R., Reiners, A., Rose, M.E., Kotani, T., Wittrock, J., Mann, A.W., Matthews, E., Latham, D.W., Barkaoui, K., Ribas, I., Gillon, M., Morales, J.C., Nowak, G., Pedraz, S., Reffert, S., Quirrenbach, A., Herrero, E., Collins, K.I., Ricker, G.R., Tamura, M., Béjar, V.J.S., Lillo-Box, J., Jenkins, J.M., Teske, J., Kemmer, J., Hirano, T., Lissauer, J.J., Plavchan, P., Schlieder, J.E., Kossakowski, D., Stock, S., El Mufti, M., Montañés-Rodríguez, P., Mori, M., Gaidos, E., De León, J.P., Benkhaldoun, Z., Oshagh, M., Schweitzer, A., Kürster, M., Narita, N., Casasayas Barris, N., Seager, S., Howell, S.B., Gonzales, E.J., Jehin, E., Kielkopf, J.F., Dreizler, S., Zechmeister, M., Hidalgo, D., Chaturvedi, P., Madrigal-Aguado, A., Matson, R.A., Lafarga, M., Amado, P.J., Essack, Z., Bauer, F.F., Kaminski, A., Law, N., Henning, T., Pollacco, D., Collins, K.A., Zohrabi, F., Cortés-Contreras, M., Pallé, E., Espinoza, N., Hesse, K., Murgas, F., Aceituno, F.J., Pozuelos, F.J., Crossfield, I.J.M., Barrado, D., Watanabe, D., Ziegler, C., Fukui, A., Hatzes, A., Twicken, J.D., Passegger, V.M., Cifuentes, C., Caldwell, D.A., Chen, G., and Luque, R.
- Abstract
We present the discovery and characterisation of two transiting planets observed by the Transiting Exoplanet Survey Satellite (TESS) orbiting the nearby (d∗ ≈ 22 pc), bright (J ≈ 9 mag) M3.5 dwarf LTT 3780 (TOI-732). We confirm both planets and their association with LTT 3780 via ground-based photometry and determine their masses using precise radial velocities measured with the CARMENES spectrograph. Precise stellar parameters determined from CARMENES high-resolution spectra confirm that LTT 3780 is a mid-M dwarf with an effective temperature of Teff = 3360 ± 51 K, a surface gravity of log g∗ = 4.81 ± 0.04 (cgs), and an iron abundance of [Fe/H] = 0.09 ± 0.16 dex, with an inferred mass of M∗ = 0.379 ± 0.016M· and a radius of R∗ = 0.382 ± 0.012R·. The ultra-short-period planet LTT 3780 b (Pb = 0.77 d) with a radius of 1.35-0.06+0.06 R·, a mass of 2.34-0.23+0.24 M·, and a bulk density of 5.24-0.81+0.94 g cm-3 joins the population of Earth-size planets with rocky, terrestrial composition. The outer planet, LTT 3780 c, with an orbital period of 12.25 d, radius of 2.42-0.10+0.10 R·, mass of 6.29-0.61+0.63 M·, and mean density of 2.45-0.37+0.44 g cm-3 belongs to the population of dense sub-Neptunes. With the two planets located on opposite sides of the radius gap, this planetary system is anexcellent target for testing planetary formation, evolution, and atmospheric models. In particular, LTT 3780 c is an ideal object for atmospheric studies with the James Webb Space Telescope (JWST).
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- 2020
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4. A super-Earth and two sub-Neptunes transiting the nearby and quiet M dwarf TOI-270
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Kavli Institute for Theoretical Physics, John Templeton Foundation, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Science and Technology Facilities Council (UK), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Ministerio de Economía y Competitividad (España), European Commission, Heising Simons Foundation, National Aeronautics and Space Administration (US), Swiss National Science Foundation, Fédération Wallonie-Bruxelles, Günther, M.N., Pozuelos, Francisco José, Dittmann, J.A., Dragomir, D., Kane, S.R., Daylan, Tansu, Feinstein, A.D., Huang, C.X., Morton, T.D., Bonfanti, A., Bouma, L.G., Burt, J., Collins, Karen A., Lissauer, J.J., Matthews, E., Montet, B.T., Vanderburg, A., Wang, Shanshan, Winters, J.G., Ricker, G.R., Vanderspek, R.K., Latham, David W., Seager, S., Winn, J.N., Jenkins, Jon M., Armstrong, J.D., Barkaoui, K., Batalha, N., Bean, J.L., Caldwell, D.A., Ciardi, D.R., Collins, K.I., Crossfield, I., Fausnaugh, Michael, Furesz, G., Gan, T., Gillon, M., Guerrero, N., Horne, K., Howell, S.B., Ireland, M., Isopi, G., Jehin, E., Kielkopf, J.F., Lepine, S., Mallia, F., Matson, R.A., Myers, G., Pallé, Enric, Suárez Yanes, Juan Carlos, Kavli Institute for Theoretical Physics, John Templeton Foundation, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Science and Technology Facilities Council (UK), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Ministerio de Economía y Competitividad (España), European Commission, Heising Simons Foundation, National Aeronautics and Space Administration (US), Swiss National Science Foundation, Fédération Wallonie-Bruxelles, Günther, M.N., Pozuelos, Francisco José, Dittmann, J.A., Dragomir, D., Kane, S.R., Daylan, Tansu, Feinstein, A.D., Huang, C.X., Morton, T.D., Bonfanti, A., Bouma, L.G., Burt, J., Collins, Karen A., Lissauer, J.J., Matthews, E., Montet, B.T., Vanderburg, A., Wang, Shanshan, Winters, J.G., Ricker, G.R., Vanderspek, R.K., Latham, David W., Seager, S., Winn, J.N., Jenkins, Jon M., Armstrong, J.D., Barkaoui, K., Batalha, N., Bean, J.L., Caldwell, D.A., Ciardi, D.R., Collins, K.I., Crossfield, I., Fausnaugh, Michael, Furesz, G., Gan, T., Gillon, M., Guerrero, N., Horne, K., Howell, S.B., Ireland, M., Isopi, G., Jehin, E., Kielkopf, J.F., Lepine, S., Mallia, F., Matson, R.A., Myers, G., Pallé, Enric, and Suárez Yanes, Juan Carlos
- Abstract
One of the primary goals of exoplanetary science is to detect small, temperate planets passing (transiting) in front of bright and quiet host stars. This enables the characterization of planetary sizes, orbits, bulk compositions, atmospheres and formation histories. These studies are facilitated by small and cool M dwarf host stars. Here we report the Transiting Exoplanet Survey Satellite (TESS) discovery of three small planets transiting one of the nearest and brightest M dwarf hosts observed to date, TOI-270 (TIC 259377017, with K-magnitude 8.3, and 22.5 parsecs away from Earth). The M3V-type star is transited by the super-Earth-sized planet TOI-270 b (1.247−0.083+0.089R) and the sub-Neptune-sized planets TOI-270 c (2.42 ± 0.13 R) and TOI-270 d (2.13 ± 0.12 R). The planets orbit close to a mean-motion resonant chain, with periods (3.36 days, 5.66 days and 11.38 days, respectively) near ratios of small integers (5:3 and 2:1). TOI-270 is a prime target for future studies because (1) its near-resonance allows the detection of transit timing variations, enabling precise mass measurements and dynamical studies; (2) its brightness enables independent radial-velocity mass measurements; (3) the outer planets are ideal for atmospheric characterization via transmission spectroscopy; and (4) the quietness of the star enables future searches for habitable zone planets. Altogether, very few systems with small, temperate exoplanets are as suitable for such complementary and detailed characterization as TOI-270.© 2019, The Author(s), under exclusive licence to Springer Nature Limited.
- Published
- 2019
5. Kepler-62 : A five-planet system with planets of 1.4 and 1.6 Earth radii in the habitable zone
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Borucki, W.J., Agol, E., Fressin, F., Kaltenegger, L., Rowe, J., Isaacson, H., Fischer, D., Batalha, N., Lissauer, J.J., Marcy, G.W., Fabrycky, D., Dxe9sert, J.-M., Bryson, S.T., Barclay, Thomas, Bastien, F., Boss, A., Brugamyer, E., Buchhave, L.A., Burke, C., Caldwell, D.A., Carter, J., Charbonneau, D., Crepp, J.R., Christensen-Dalsgaard, J., Christiansen, J.L., Ciardi, D., Cochran, W.D., DeVore, E., Doyle, L., Dupree, A.K., Endl, M., Everett, M.E., Ford, E.B., Fortney, J., Gautier III, T.N., Geary, et al., Borucki, W.J., Agol, Fressin, Kaltenegger, Rowe, Isaacson, Fischer, Batalha, Lissauer, J.J., Marcy, G.W., Fabrycky, Dxe9sert, J.-M., Bryson, S.T., Barclay, Thomas, Bastien, Boss, Brugamyer, Buchhave, L.A., Burke, Caldwell, D.A., Carter, Charbonneau, Crepp, J.R., Christensen-Dalsgaard, Christiansen, J.L., Ciardi, Cochran, W.D., DeVore, Doyle, Dupree, A.K., Endl, Everett, M.E., Ford, E.B., Fortney, Gautier III, T.N., and Geary
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- 2013
6. Search for small trans-Neptunian objects by the TAOS project
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Chen, W.P., primary, Alcock, C., additional, Axelrod, T., additional, Bianco, F.B., additional, Byun, Y.I., additional, Chang, Y.H., additional, Cook, K.H., additional, Dave, R., additional, Giammarco, J., additional, Kim, D.W., additional, King, S.K., additional, Lee, T., additional, Lehner, M., additional, Lin, C.C., additional, Lin, H.C., additional, Lissauer, J.J., additional, Marshall, S., additional, Meinshausen, N., additional, Mondal, S., additional, de Pater, I., additional, Porrata, R., additional, Rice, J., additional, Schwamb, M.E., additional, Wang, A., additional, Wang, S.Y., additional, Wen, C.Y., additional, and Zhang, Z.W., additional
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- 2006
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7. The Titan-1:0 nodal bending wave in Saturn's.
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Rosen, P.A. and Lissauer, J.J.
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TITAN (Satellite) - Abstract
Report on an oscillatory feature observed in the Voyager 1 radio occultation of Saturn's rings (Ring C) identified as a one-armed spiral bending wave excited by Titan's-1:0 nodal inner vertical resonance.
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- 1988
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