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3 results on '"Lam KWF"'

1. TOI-1268b: The youngest hot Saturn-mass transiting exoplanet

Author

Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Subjak, J, Endl, M, Chaturvedi, P, Karjalainen, R, Cochran, WD, Esposito, M, Gandolfi, D, Lam, KWF, Stassun, K, Zák, J, Lodieu, N, Boffin, HMJ, MacQueen, PJ, Hatzes, A, Guenther, EW, Georgieva, I, Grziwa, S, Schmerling, H, Skarka, M, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Subjak, J, Endl, M, Chaturvedi, P, Karjalainen, R, Cochran, WD, Esposito, M, Gandolfi, D, Lam, KWF, Stassun, K, Zák, J, Lodieu, N, Boffin, HMJ, MacQueen, PJ, Hatzes, A, Guenther, EW, Georgieva, I, Grziwa, S, Schmerling, H, and Skarka, M

Abstract

We report the discovery of TOI-1268b, a transiting Saturn-mass planet from the TESS space mission. With an age of less than 1 Gyr, derived from various age indicators, TOI-1268b is the youngest Saturn-mass planet known to date; it contributes to the small sample of well-characterised young planets. It has an orbital period of P = 8.1577080 ± 0.0000044 days, and transits an early K-dwarf star with a mass of M? = 0.96 ± 0.04 M , a radius of R? = 0.92 ± 0.06 R , an effective temperature of Teff = 5300 ± 100 K, and a metallicity of 0.36 ± 0.06 dex. By combining TESS photometry with high-resolution spectra acquired with the Tull spectrograph at the McDonald Observatory, and the high-resolution spectrographs at the Tautenburg and Ondˇrejov Observatories, we measured a planetary mass of Mp = 96.4 ± 8.3 M⊕ and a radius of Rp = 9.1 ± 0.6 R⊕. TOI-1268 is an ideal system for studying the role of star-planet tidal interactions for non-inflated Saturn-mass planets. We used system parameters derived in this paper to constrain the planet’s tidal quality factor to the range of 104.5−5.3 . When compared with the sample of other non-inflated Saturn-mass planets, TOI-1268b is one of the best candidates for transmission spectroscopy studies.

Published
2023

2. A resonant sextuplet of sub-Neptunes transiting the bright star HD 110067.

Author

Luque R, Osborn HP, Leleu A, Pallé E, Bonfanti A, Barragán O, Wilson TG, Broeg C, Cameron AC, Lendl M, Maxted PFL, Alibert Y, Gandolfi D, Delisle JB, Hooton MJ, Egger JA, Nowak G, Lafarga M, Rapetti D, Twicken JD, Morales JC, Carleo I, Orell-Miquel J, Adibekyan V, Alonso R, Alqasim A, Amado PJ, Anderson DR, Anglada-Escudé G, Bandy T, Bárczy T, Barrado Navascues D, Barros SCC, Baumjohann W, Bayliss D, Bean JL, Beck M, Beck T, Benz W, Billot N, Bonfils X, Borsato L, Boyle AW, Brandeker A, Bryant EM, Cabrera J, Carrazco-Gaxiola S, Charbonneau D, Charnoz S, Ciardi DR, Cochran WD, Collins KA, Crossfield IJM, Csizmadia S, Cubillos PE, Dai F, Davies MB, Deeg HJ, Deleuil M, Deline A, Delrez L, Demangeon ODS, Demory BO, Ehrenreich D, Erikson A, Esparza-Borges E, Falk B, Fortier A, Fossati L, Fridlund M, Fukui A, Garcia-Mejia J, Gill S, Gillon M, Goffo E, Gómez Maqueo Chew Y, Güdel M, Guenther EW, Günther MN, Hatzes AP, Helling C, Hesse KM, Howell SB, Hoyer S, Ikuta K, Isaak KG, Jenkins JM, Kagetani T, Kiss LL, Kodama T, Korth J, Lam KWF, Laskar J, Latham DW, Lecavelier des Etangs A, Leon JPD, Livingston JH, Magrin D, Matson RA, Matthews EC, Mordasini C, Mori M, Moyano M, Munari M, Murgas F, Narita N, Nascimbeni V, Olofsson G, Osborne HLM, Ottensamer R, Pagano I, Parviainen H, Peter G, Piotto G, Pollacco D, Queloz D, Quinn SN, Quirrenbach A, Ragazzoni R, Rando N, Ratti F, Rauer H, Redfield S, Ribas I, Ricker GR, Rudat A, Sabin L, Salmon S, Santos NC, Scandariato G, Schanche N, Schlieder JE, Seager S, Ségransan D, Shporer A, Simon AE, Smith AMS, Sousa SG, Stalport M, Szabó GM, Thomas N, Tuson A, Udry S, Vanderburg AM, Van Eylen V, Van Grootel V, Venturini J, Walter I, Walton NA, Watanabe N, Winn JN, and Zingales T

Abstract

Planets with radii between that of the Earth and Neptune (hereafter referred to as 'sub-Neptunes') are found in close-in orbits around more than half of all Sun-like stars 1,2 . However, their composition, formation and evolution remain poorly understood 3 . The study of multiplanetary systems offers an opportunity to investigate the outcomes of planet formation and evolution while controlling for initial conditions and environment. Those in resonance (with their orbital periods related by a ratio of small integers) are particularly valuable because they imply a system architecture practically unchanged since its birth. Here we present the observations of six transiting planets around the bright nearby star HD 110067. We find that the planets follow a chain of resonant orbits. A dynamical study of the innermost planet triplet allowed the prediction and later confirmation of the orbits of the rest of the planets in the system. The six planets are found to be sub-Neptunes with radii ranging from 1.94R ⊕ to 2.85R ⊕ . Three of the planets have measured masses, yielding low bulk densities that suggest the presence of large hydrogen-dominated atmospheres., (© 2023. The Author(s), under exclusive licence to Springer Nature Limited.)

Published
2023
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3. GJ 367b: A dense, ultrashort-period sub-Earth planet transiting a nearby red dwarf star.

Author

Lam KWF, Csizmadia S, Astudillo-Defru N, Bonfils X, Gandolfi D, Padovan S, Esposito M, Hellier C, Hirano T, Livingston J, Murgas F, Smith AMS, Collins KA, Mathur S, Garcia RA, Howell SB, Santos NC, Dai F, Ricker GR, Vanderspek R, Latham DW, Seager S, Winn JN, Jenkins JM, Albrecht S, Almenara JM, Artigau E, Barragán O, Bouchy F, Cabrera J, Charbonneau D, Chaturvedi P, Chaushev A, Christiansen JL, Cochran WD, De Meideiros JR, Delfosse X, Díaz RF, Doyon R, Eigmüller P, Figueira P, Forveille T, Fridlund M, Gaisné G, Goffo E, Georgieva I, Grziwa S, Guenther E, Hatzes AP, Johnson MC, Kabáth P, Knudstrup E, Korth J, Lewin P, Lissauer JJ, Lovis C, Luque R, Melo C, Morgan EH, Morris R, Mayor M, Narita N, Osborne HLM, Palle E, Pepe F, Persson CM, Quinn SN, Rauer H, Redfield S, Schlieder JE, Ségransan D, Serrano LM, Smith JC, Šubjak J, Twicken JD, Udry S, Van Eylen V, and Vezie M

Abstract

Ultrashort-period (USP) exoplanets have orbital periods shorter than 1 day. Precise masses and radii of USP exoplanets could provide constraints on their unknown formation and evolution processes. We report the detection and characterization of the USP planet GJ 367b using high-precision photometry and radial velocity observations. GJ 367b orbits a bright ( V -band magnitude of 10.2), nearby, and red (M-type) dwarf star every 7.7 hours. GJ 367b has a radius of 0.718 ± 0.054 Earth-radii and a mass of 0.546 ± 0.078 Earth-masses, making it a sub-Earth planet. The corresponding bulk density is 8.106 ± 2.165 grams per cubic centimeter—close to that of iron. An interior structure model predicts that the planet has an iron core radius fraction of 86 ± 5%, similar to that of Mercury’s interior.

Published
2021
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