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Author Asenjo, F.A.; Hojman, S.A.
Title Class of Exact Solutions for a Cosmological Model of Unified Gravitational and Quintessence Fields Type
Year 2017 Publication Foundations Of Physics Abbreviated Journal Found. Phys.
Volume 47 Issue 7 Pages 887-896
Keywords Quintessence; Exact solution; Unification of geometry and dark matter
Abstract A new approach to tackle Einstein equations for an isotropic and homogeneous Friedmann-Robertson-Walker Universe in the presence of a quintessence scalar field is devised. It provides a way to get a simple exact solution to these equations. This solution determines the quintessence potential uniquely and it differs from solutions which have been used to study inflation previously. It relays on a unification of geometry and dark matter implemented through the definition of a functional relation between the scale factor of the Universe and the quintessence field. For a positive curvature Universe, this solution produces perpetual accelerated expansion rate of the Universe, while the Hubble parameter increases abruptly, attains a maximum value and decreases thereafter. The behavior of this cosmological solution is discussed and its main features are displayed. The formalism is extended to include matter and radiation.
Address [Asenjo, Felipe A.] Univ Adolfo Ibanez, Fac Ingn & Ciencias, Santiago, Chile, Email: felipe.asenjo@uai.cl;
Corporate Author Thesis
Publisher Springer Place of Publication Editor
Language English Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0015-9018 ISBN Medium
Area Expedition Conference
Notes WOS:000404224500003 Approved
Call Number UAI @ eduardo.moreno @ Serial 741
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Author Heitzmann, A.; Zhou, G.; Quinn, S.N.; Huang, C.X.; Dong, J.Y.; Bouma, L.G.; Dawson, R.I.; Marsden, S.C.; Wright, D.; Petit, P.; Collins, K.A.; Barkaoui, K.; Wittenmyer, R.A.; Gillen, E.; Brahm, R.; Hobson, M.; Hellier, C.; Ziegler, C.; Briceno, C.; Law, N.; Mann, A.W.; Howell, S.B.; Gnilka, C.L.; Littlefield, C.; Latham, D.W.; Lissauer, J.J.; Newton, E.R.; Krolikowski, D.M.; Kerr, R.; Rampalli, R.; Douglas, S.T.; Eisner, N.L.; Guedj, N.; Sun, G.Y.; Smit, M.; Huten, M.; Eschweiler, T.; Abe, L.; Guillot, T.; Ricker, G.; Vanderspek, R.; Seager, S.; Jenkins, J.M.; Ting, E.B.; Winn, J.N.; Ciardi, D.R.; Vanderburg, A.M.; Burke, C.J.; Rodriguez, D.R.; Daylan, T.
Title TOI-4562b: A Highly Eccentric Temperate Jupiter Analog Orbiting a Young Field Star Type
Year 2023 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 165 Issue 3 Pages 121
Keywords K2 ROTATION PERIOD; SOLD TRANSITING HOT; LOW-MASS HYADS; TESS HUNT; GIANT PLANETS; STELLAR SPECTRA; WARM JUPITERS; LIGHT CURVES; SIZED PLANET; SURVEY. II.
Abstract We report the discovery of TOI-4562b (TIC-349576261), a Jovian planet orbiting a young F7V-type star, younger than the Praesepe/Hyades clusters (< 700 Myr). This planet stands out because of its unusually long orbital period for transiting planets with known masses (Porb = 225.11781(- 0.00022) (+0.00025 )days) and because it has a substantial eccentricity (e = 0.76(- 0.02) (+0.02)). The location of TOI-4562 near the southern continuous viewing zone of TESS allowed observations throughout 25 sectors, enabling an unambiguous period measurement from TESS alone. Alongside the four available TESS transits, we performed follow-up photometry using the South African Astronomical Observatory node of the Las Cumbres Observatory and spectroscopy with the CHIRON spectrograph on the 1.5 m SMARTS telescope. We measure a radius of 1.118 (+0.013) (-0.014) R(J )and a mass of 2.30(-0.47)(+0.48)M(J) for TOI-4562b. The radius of the planet is consistent with contraction models describing the early evolution of the size of giant planets. We detect tentative transit timing variations at the similar to 20 minutes level from five transit events, favoring the presence of a companion that could explain the dynamical history of this system if confirmed by future follow-up observations. With its current orbital configuration, tidal timescales are too long for TOI-4562b to become a hot Jupiter via high eccentricity migration though it is not excluded that interactions with the possible companion could modify TOI4562b's eccentricity and trigger circularization. The characterization of more such young systems is essential to set constraints on models describing giant-planet evolution.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000940570300001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1759
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Author Hobson, M.J.; Jordan, A.; Bryant, E.M.; Brahm, R.; Bayliss, D.; Hartman, J.D.; Bakos, G.A.; Henning, T.; Almenara, J.M.; Barkaoui, K.; Benkhaldoun, Z.; Bonfils, X.; Bouchy, F.; Charbonneau, D.; Cointepas, M.; Collins, K.A.; Eastman, J.D.; Ghachoui, M.; Gillon, M.; Goeke, R.F.; Horne, K.; Irwin, J.M.; Jehin, E.; Jenkins, J.M.; Latham, D.W.; Moldovan, D.; Murgas, F.; Pozuelos, F.J.; Ricker, G.R.; Schwarz, R.P.; Seager, S.; Srdoc, G.; Striegel, S.; Timmermans, M.; Vanderburg, A.; Vanderspek, R.; Winn, J.N.
Title TOI-3235 b: A Transiting Giant Planet around an M4 Dwarf Star Type
Year 2023 Publication Astrophysical Journal Letters Abbreviated Journal Astrophys. J. Lett.
Volume 946 Issue 1 Pages L4
Keywords LIMB-DARKENING COEFFICIENT; SLOW-MASS STAR; METALLICITY RELATION; ERROR-CORRECTION; MESA ISOCHRONES; K KEPLER; ALGORITHM; SEARCH; TESS; II
Abstract We present the discovery of TOI-3235 b, a short-period Jupiter orbiting an M dwarf with a stellar mass close to the critical mass at which stars transition from partially to fully convective. TOI-3235 b was first identified as a candidate from TESS photometry and confirmed with radial velocities from ESPRESSO and ground-based photometry from HATSouth, MEarth-South, TRAPPIST-South, LCOGT, and ExTrA. We find that the planet has a mass of 0.665 +/- 0.025 M-J and a radius of 1.017 +/- 0.044 R-J. It orbits close to its host star, with an orbital period of 2.5926 days but has an equilibrium temperature of approximate to 604 K, well below the expected threshold for radius inflation of hot Jupiters. The host star has a mass of 0.3939 +/- 0.0030 M-circle dot, a radius of 0.3697 +/- 0.0018 R-circle dot;, an effective temperature of 3389 K, and a J-band magnitude of 11.706 +/- 0.025. Current planet formation models do not predict the existence of gas giants such as TOI-3235 b around such low-mass stars. With a high transmission spectroscopy metric, TOI-3235 b is one of the best-suited giants orbiting M dwarfs for atmospheric characterization.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 2041-8205 ISBN Medium
Area Expedition Conference
Notes WOS:000956092700001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1834
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Author Leleu, A.; Alibert, Y.; Hara, N.C.; Hooton, M. J.; Wilson, T.G.; Robutel, P.; Delisle, J.B.; Laskar, J .; Hoyer, S.; Lovis, C.; Bryant, E.M.; Ducrot, E.; Cabrera, J.; Delrez, L.; Acton, J.S.; Adibekyan, V.; Allart, R.; Prieto, C.A.; Alonso, R.; Alves, D.; Anderson, D.R.; Angerhausen, D.; Escude, G.A.; Asquier, J.; Barrado, D.; Barros, S.C.C.; Baumjohann, W.; Bayliss, D.; Beck, M.; Beck, T.; Bekkelien, A.; Benz, W.; Billot, N.; Bonfanti, A.; Bonfils, X.; Bouchy, F.; Bourrier, V.; Boue, G.; Brandeker, A.; Broeg, C.; Buder, M.; Burdanov, A.; Burleigh, M.R.; Barczy, T.; Cameron, A.C.; Chamberlain, S.; Charnoz, S.; Cooke, B.F.; Van Damme, C.C.; Correia, A.C.M.; Cristiani, S.; Damasso, M.; Davies, M.B.; Deleuil, M.; Demangeon, O.D.S.; Demory, B.O.; Di Marcantonio, P.; Di Persio, G.; Dumusque, X.; Ehrenreich, D.; Erikson, A.; Figueira, P.; Fortier, A.; Fossati, L.; Fridlund, M.; Futyan, D.; Gandolfi, D.; Munoz, A.G.; Garcia, L.J.; Gill, S.; Osorio, M.R.Z.; Gillen, E.; Gillon, M.; Goad, M.R.; Hernandez, J.I.G.; Guedel, M.; Haldemann, J.; Henderson, B.; Heng, K.; Hogan, A.E.; Isaak, K.; Jehin, E.; Jenkins, J.S.; Jordan, A.; Kiss, L.; Kristiansen, M.H.; Lam, K.; Lavie, B.; des Etangs, A.L.; Lendl, M.; Lillo-Box, J.; Lo Curto, G.; Magrin, D.; Martins, C.J.A.P.; Maxted, P.F.L.; McCormac, J.; Mehner, A.; Micela, G.; Molaro, P.; Moyano, M.; Murray, C.A.; Nascimbeni, V.; Nunes, N.J.; Olofsson, G.; Osborn, H.P.; Oshagh, M.; Ottensamer, R.; Pagano, I.; Palle, E.; Pedersen, P.P.; Pepe, F.A.; Persson, C.M.; Peter, G.; Piotto, G.; Polenta, G.; Pollacco, D.; Poretti, E.; Pozuelos, F.J.; Queloz, D.; Ragazzoni, R.; Rando, N.; Ratti, F.; Rauer, H.; Raynard, L.; Rebolo, R.; Reimers, C.; Ribas, I.; Santos, N.C.; Scandariato, G.; Schneider, J.; Sebastian, D.; Sestovic, M.; Simon, A.E.; Smith, A.M.S.; Sousa, S.G.; Sozzetti, A.; Steller, M.; Mascareno, A.S.; Szabo, G.M.; Segransan, D.; Thomas, N.; Thompson, S.; Tilbrook, R.H.; Triaud, A.; Turner, O.; Udry, S.; Van Grootel, V.; Venus, H.; Verrecchia, F.; Vines, J.I.; Walton, N.A.; West, R.G.; Wheatley, P.J.; Wolter, D.
Title Six transiting planets and a chain of Laplace resonances in TOI-178 Type
Year 2021 Publication Astronomy & Astrophysics Abbreviated Journal Astron. Astrophys.
Volume 649 Issue Pages A26
Keywords HOT SUPER-EARTHS; TESS INPUT CATALOG; RADIUS DISTRIBUTION; MASS; SYSTEM; MODEL; STARS; MIGRATION; DYNAMICS; TOOL
Abstract Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. In this context, TOI-178 has been the subject of particular attention since the first TESS observations hinted at the possible presence of a near 2:3:3 resonant chain. Here we report the results of observations from CHEOPS, ESPRESSO, NGTS, and SPECULOOS with the aim of deciphering the peculiar orbital architecture of the system. We show that TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, with radii ranging from

1.152(-0.070)(+0.073)</textual-form>

1.152-0.070+0.073 to

2.87(-0.13)(+0.14)</textual-form> 2.87-0.13+0.14 Earth radii and periods of 1.91, 3.24, 6.56, 9.96, 15.23, and 20.71 days. All planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet, jumping from

1.02(-0.23)(+0.28)</textual-form> 1.02-0.23+0.28 to

0.177(-0.061)(+0.055)</textual-form> 0.177-0.061+0.055 times the Earth's density between planets c and d. Using Bayesian interior structure retrieval models, we show that the amount of gas in the planets does not vary in a monotonous way, contrary to what one would expect from simple formation and evolution models and unlike other known systems in a chain of Laplace resonances. The brightness of TOI-178 (H = 8.76 mag, J = 9.37 mag, V = 11.95 mag) allows for a precise characterisation of its orbital architecture as well as of the physical nature of the six presently known transiting planets it harbours. The peculiar orbital configuration and the diversity in average density among the planets in the system will enable the study of interior planetary structures and atmospheric evolution, providing important clues on the formation of super-Earths and mini-Neptunes.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6361 ISBN Medium
Area Expedition Conference
Notes WOS:000655036600001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1416
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Author Trifonov, T.; Brahm, R.; Espinoza, N.; Henning, T.; Jordan, A.; Nesvorny, D.; Dawson, R.I.; Lissauer, J.J.; Lee, M.H.; Kossakowski, D.; Rojas, F.I.; Hobson, M.J.; Sarkis, P.; Schlecker, M.; Bitsch, B.; Bakos, G.A.; Barbieri, M.; Bhatti, W.; Butler, R.P.; Crane, J.D.; Nandakumar, S.; Diaz, M.R.; Shectman, S.; Teske, J.; Torres, P.; Suc, V.; Vines, J.I.; Wang, S.R.X.; Ricker, G.R.; Shporer, A.; Vanderburg, A.; Dragomir, D.; Vanderspek, R.; Burke, C.J.; Daylan, T.; Shiao, B.; Jenkins, J.M.; Wohler, B.; Seager, S.; Winn, J.N.
Title A Pair of Warm Giant Planets near the 2:1 Mean Motion Resonance around the K-dwarf Star TOI-2202* Type
Year 2021 Publication Astronomical Journal Abbreviated Journal Astron. J.
Volume 162 Issue 6 Pages 283
Keywords EARTH-SIZED PLANET; SUPER-EARTH; HOT JUPITERS; TESS; SYSTEMS; TRANSIT; NEPTUNE; MODEL; PERIODOGRAM; SCATTERING
Abstract TOI-2202 b is a transiting warm Jovian-mass planet with an orbital period of P = 11.91 days identified from the Full Frame Images data of five different sectors of the TESS mission. Ten TESS transits of TOI-2202 b combined with three follow-up light curves obtained with the CHAT robotic telescope show strong transit timing variations (TTVs) with an amplitude of about 1.2 hr. Radial velocity follow-up with FEROS, HARPS, and PFS confirms the planetary nature of the transiting candidate (a (b) = 0.096 +/- 0.001 au, m (b) = 0.98 +/- 0.06 M (Jup)), and a dynamical analysis of RVs, transit data, and TTVs points to an outer Saturn-mass companion (a (c) = 0.155 +/- 0.002 au, m (c) = 0.37 +/- 0.10 M (Jup)) near the 2:1 mean motion resonance. Our stellar modeling indicates that TOI-2202 is an early K-type star with a mass of 0.82 M (circle dot), a radius of 0.79 R (circle dot), and solar-like metallicity. The TOI-2202 system is very interesting because of the two warm Jovian-mass planets near the 2:1 mean motion resonance, which is a rare configuration, and their formation and dynamical evolution are still not well understood.
Address
Corporate Author Thesis
Publisher Place of Publication Editor
Language Summary Language Original Title
Series Editor Series Title Abbreviated Series Title
Series Volume Series Issue Edition
ISSN 0004-6256 ISBN Medium
Area Expedition Conference
Notes WOS:000725244600001 Approved
Call Number UAI @ alexi.delcanto @ Serial 1511
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