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| Author |
Bergmann, C.; Jones, MI.; Zhao, J.; Mustill, AJ.; Brahm, R.; Torres, P.; Wittenmyer, RA.; Gunn, F.; Pollard, KR.; Zapata, A.; Vanzi, L.; Wang, SH. |
| Title |
HD 76920 b pinned down: A detailed analysis of the most eccentric planetary system around an evolved star |
Type |
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| Year |
2021 |
Publication |
Publications of the Astronomical Society of Australia |
Abbreviated Journal |
PUBL. ASTRON. SOC. AUST. |
| Volume |
38 |
Issue |
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Pages |
e019 |
| Keywords |
EXTRA-SOLAR PLANETS; RADIAL-VELOCITY; GIANT STAR; STELLAR EVOLUTION; MASS COMPANION; EXOPLANETS; PRECISION; SEARCH; TRANSIT; I. |
| Abstract |
We present 63 new multi-site radial velocity (RV) measurements of the K1III giant HD 76920, which was recently reported to host the most eccentric planet known to orbit an evolved star. We focused our observational efforts on the time around the predicted periastron passage and achieved near-continuous phase coverage of the corresponding RV peak. By combining our RV measurements from four different instruments with previously published ones, we confirm the highly eccentric nature of the system and find an even higher eccentricity of , an orbital period of 415.891(-0.039)(+0.043) d, and a minimum mass of 3.13(-0.43)(+0.41) M-J for the planet. The uncertainties in the orbital elements are greatly reduced, especially for the period and eccentricity. We also performed a detailed spectroscopic analysis to derive atmospheric stellar parameters, and thus the fundamental stellar parameters (M-*, R-*, L-*) taking into account the parallax from Gaia DR2, and independently determined the stellar mass and radius using asteroseismology. Intriguingly, at periastron, the planet comes to within 2.4 stellar radii of its host star's surface. However, we find that the planet is not currently experiencing any significant orbital decay and will not be engulfed by the stellar envelope for at least another 50-80 Myr. Finally, while we calculate a relatively high transit probability of 16%, we did not detect a transit in the TESS photometry. |
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1323-3580 |
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WOS:000642222500001 |
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UAI @ alexi.delcanto @ |
Serial |
1379 |
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| Author |
Carmichael, T.W.; Quinn, S.N.; Mustill, A.J.; Huang, C.; Zhou, G.; Persson, C.M.; Nielsen, L.D.; Collins, K.A.; Ziegler, C.; Collins, K.I.; Rodriguez, J.E.; Shporer, A.; Brahm, R.; Mann, A.W.; Bouchy, F.; Fridlund, M.; Stassun, K.G.; Hellier, C.; Seidel, J.V.; Stalport, M.; Udry, S.; Pepe, F.; Ireland, M.; Zerjal, M.; Briceno, C.; Law, N.; Jordan, A.; Espinoza, N.; Henning, T.; Sarkis, P.; Latham, D.W. |
| Title |
Two Intermediate-mass Transiting Brown Dwarfs from the TESS Mission |
Type |
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| Year |
2020 |
Publication |
Astronomical Journal |
Abbreviated Journal |
Astron. J. |
| Volume |
160 |
Issue |
1 |
Pages |
15 pp |
| Keywords |
Brown dwarfs; Radial velocity; Transit photometry; Spectroscopy; Photometry; Substellar companion stars |
| Abstract |
We report the discovery of two intermediate-mass transiting brown dwarfs (BDs), TOI-569b and TOI-1406b, from NASA's Transiting Exoplanet Survey Satellite mission. TOI-569b has an orbital period of P = 6.55604 0.00016 days, a mass of M-b = 64.1 1.9 , and a radius of R-b = 0.75 0.02 . Its host star, TOI-569, has a mass of M-star = 1.21 0.05, a radius of R-star = 1.47 0.03 dex, and an effective temperature of T-eff = 5768 110 K. TOI-1406b has an orbital period of P = 10.57415 0.00063 days, a mass of M-b = 46.0 2.7 , and a radius of R-b = 0.86 0.03 . The host star for this BD has a mass of M-star = 1.18 0.09 a radius of R-star = 1.35 0.03 dex, and an effective temperature of T-eff = 6290 100 K. Both BDs are in circular orbits around their host stars and are older than 3 Gyr based on stellar isochrone models of the stars. TOI-569 is one of two slightly evolved stars known to host a transiting BD (the other being KOI-415). TOI-1406b is one of three known transiting BDs to occupy the mass range of 40-50 and one of two to have a circular orbit at a period near 10 days (with the first being KOI-205b). Both BDs have reliable ages from stellar isochrones, in addition to their well-constrained masses and radii, making them particularly valuable as tests for substellar isochrones in the BD mass-radius diagram. |
| Address |
[Carmichael, Theron W.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA, Email: tcarmich@cfa.harvard.edu |
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Iop Publishing Ltd |
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English |
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0004-6256 |
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| Notes |
WOS:000549117200001 |
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UAI @ eduardo.moreno @ |
Serial |
1179 |
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Eberhardt, J.; Trifonov, T.; Kurster, M.; Stock, S.; Henning, T.; Wollbold, A.; Reffert, S.; Lee, M.H.; Zechmeister, M.; Rodler, F.; Zakhozhay, O.; Heeren, P.; Gandolfi, D.; Barragan, O.; Pinto, M.T.; Wolthoff, V.; Sarkis, P.; Brems, S.S. |
| Title |
Dynamical Architecture of the HD 107148 Planetary System |
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| Year |
2022 |
Publication |
Astronomical Journal |
Abbreviated Journal |
Astron. J. |
| Volume |
163 |
Issue |
5 |
Pages |
198 |
| Keywords |
LOMB-SCARGLE PERIODOGRAM; EXTRA-SOLAR PLANETS; RADIAL-VELOCITIES; ORBITAL SOLUTIONS; CARMENES SEARCH; M DWARFS; COMPANIONS; PRECISION; STARS; EXOPLANETS |
| Abstract |
We present an independent Doppler validation and dynamical orbital analysis of the two-planet system HD 107148, which was recently announced in Rosenthal et al. Our detailed analyses are based on literature HIRES data and newly obtained HARPS and CARMENES radial-velocity (RV) measurements as part of our survey in search for additional planets around single-planet systems. We perform a periodogram analysis of the available HIRES and HARPS precise RVs and stellar activity indicators. We do not find any apparent correlation between the RV measurements and the stellar activity indicators, thus linking the two strong periodicities to a moderately compact multiplanet system. We carry out orbital fitting analysis by testing various one- and two-planet orbital configurations and studying the posterior probability distribution of the fitted parameters. Our results solidify the existence of a Saturn-mass planet (HD 107148b, discovered first) with a period of P (b) similar to 77.2 days and a second, eccentric (e (c) similar to 0.4), Neptune-mass exoplanet (HD 107148c) with an orbital period of P (c) similar to 18.3 days. Finally, we investigate the two-planet system's long-term stability and overall orbital dynamics with the posterior distribution of our preferred orbital configuration. Our N-body stability simulations show that the system is long-term stable and exhibits large secular osculations in eccentricity but in no particular mean motion resonance configuration. The HD 107148 system, consisting of a solar-type main-sequence star with two giant planets in a rare configuration, features a common proper-motion white dwarf companion and is therefore a valuable target for understanding the formation and evolution of planetary systems. |
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0004-6256 |
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WOS:000778725000001 |
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UAI @ alexi.delcanto @ |
Serial |
1562 |
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Espinoza-Retamal, J.I.; Brahm, R.; Petrovich, C.; Jordán, A.; Stefánsson, G.; Sedaghati, E.; Hobson, M.J.; Muñoz, D.J.; Boyle, G.; Leiva, R.; Suc, V. |
| Title |
The Aligned Orbit of the Eccentric Proto Hot Jupiter TOI-3362b |
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| Year |
2023 |
Publication |
Astrophysical Journal Letters |
Abbreviated Journal |
Astrophys. J. Lett. |
| Volume |
958 |
Issue |
2 |
Pages |
L20 |
| Keywords |
IN-SITU FORMATION; PLANET; TRANSIT; EVOLUTION; BINARY; PHOTOMETRY; SCATTERING; TELESCOPE; MIGRATION; COMPANION |
| Abstract |
High-eccentricity tidal migration predicts the existence of highly eccentric proto hot Jupiters on the “tidal circularization track,” meaning that they might eventually become hot Jupiters, but that their migratory journey remains incomplete. Having experienced moderate amounts of tidal evolution of their orbital elements, proto hot Jupiter systems can be powerful test beds for the underlying mechanisms of eccentricity growth. Notably, they may be used for discriminating between variants of high-eccentricity migration, each predicting a distinct evolution of misalignment between the star and the planet's orbit. We constrain the spin-orbit misalignment of the proto hot Jupiter TOI-3362b with high-precision radial-velocity observations using ESPRESSO at Very Large Telescope. The observations reveal a sky-projected obliquity lambda=1.2+2.8(degrees)/-2.7 and constrain the orbital eccentricity to e = 0.720 +/- 0.016, making it one of the most eccentric gas giants for which the obliquity has been measured. Although the large eccentricity and the striking orbit alignment of the planet are puzzling, we suggest that ongoing coplanar high-eccentricity migration driven by a distant companion is a possible explanation for the system's architecture. This distant companion would need to reside beyond 5 au at 95% confidence to be compatible with the available radial-velocity observations. |
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2041-8205 |
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WOS:001109357900001 |
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UAI @ alexi.delcanto @ |
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1929 |
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