2020NatAs...4.1148J


Query : 2020NatAs...4.1148J

2020NatAs...4.1148J - Nature Astronomy, 4, 1148-1157 (2020/December-0)

An ultrahot Neptune in the Neptune desert.

JENKINS J.S., DIAZ M.R., KURTOVIC N.T., ESPINOZA N., VINES J.I., ROJAS P.A.P., BRAHM R., TORRES P., CORTES-ZULETA P., SOTO M.G., LOPEZ E.D., KING G.W., WHEATLEY P.J., WINN J.N., CIARDI D.R., RICKER G., VANDERSPEK R., LATHAM D.W., SEAGER S., JENKINS J.M., BEICHMAN C.A., BIERYLA A., BURKE C.J., CHRISTIANSEN J.L., HENZE C.E., KLAUS T.C., McCAULIFF S., MORI M., NARITA N., NISHIUMI T., TAMURA M., DE LEON J.P., QUINN S.N., VILLASENOR J.N., VEZIE M., LISSAUER J.J., COLLINS K.A., COLLINS K.I., ISOPI G., MALLIA F., ERCOLINO A., PETROVICH C., JORDAN A., ACTON J.S., ARMSTRONG D.J., BAYLISS D., BOUCHY F., BELARDI C., BRYANT E.M., BURLEIGH M.R., CABRERA J., CASEWELL S.L., CHAUSHEV A., COOKE B.F., EIGMULLER P., ERIKSON A., FOXELL E., GANSICKE B.T., GILL S., GILLEN E., GUNTHER M.N., GOAD M.R., HOOTON M.J., JACKMAN J.A.G., LOUDEN T., McCORMAC J., MOYANO M., NIELSEN L.D., POLLACCO D., QUELOZ D., RAUER H., RAYNARD L., SMITH A.M.S., TILBROOK R.H., TITZ-WEIDER R., TURNER O., UDRY S., WALKER S.R., WATSON C.A., WEST R.G., PALLE E., ZIEGLER C., LAW N. and MANN A.W.

Abstract (from CDS):

About 1 out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultrashort-period planet1,2. All of the previously known ultrashort-period planets are either hot Jupiters, with sizes above 10 Earth radii (R⊕), or apparently rocky planets smaller than 2 R⊕. Such lack of planets of intermediate size (the `hot Neptune desert') has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here we report the discovery of an ultrashort-period planet with a radius of 4.6 R⊕ and a mass of 29 M⊕, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite3 revealed transits of the bright Sun-like star LTT 9779 every 0.79 days. The planet's mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0-2.9+2.7?% of the total mass. With an equilibrium temperature around 2,000 K, it is unclear how this `ultrahot Neptune' managed to retain such an envelope. Follow-up observations of the planet's atmosphere to better understand its origin and physical nature will be facilitated by the star's brightness (Vmag = 9.8).

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Journal keyword(s):

Status at CDS : Large table(s) will be appraised for possible ingestion in VizieR.

Simbad objects: 15

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Number of rows : 15
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 HD 3167b Pl 00 34 57.5242131960 +04 22 53.284093032           ~ 64 0
2 K2-106b Pl 00 52 19.1415736296 +10 47 40.906374828           ~ 51 0
3 HD 10069b Pl 01 37 25.0332798696 -45 40 40.374717456           ~ 364 1
4 NGTS-4b Pl 05 58 23.7549496011 -30 48 42.363268864           ~ 33 0
5 CoRoT-7b Pl 06 43 49.4690164104 -01 03 46.826642700           ~ 401 1
6 * rho01 Cnc e Pl 08 52 35.8111044043 +28 19 50.954994470           ~ 572 1
7 WASP-43 * 10 19 38.0088913464 -09 48 22.605801336   13.782 12.490 12.022 11.10 K7V 144 2
8 K2-131b Pl 12 11 00.3783875832 -09 45 54.781040484           ~ 23 0
9 BD-05 3504b Pl 12 27 29.5846968120 -06 43 18.766944228           ~ 43 0
10 Kepler-10b Pl 19 02 43.0613892904 +50 14 28.701617339           ~ 295 1
11 Kepler-78b Pl 19 34 58.0137407208 +44 26 53.960186940           ~ 140 1
12 WASP-47e Pl 22 04 48.7261549272 -12 01 07.998743676           ~ 72 0
13 K2-141b Pl 23 23 39.9709098120 -01 11 21.448681332           ~ 66 0
14 CD-38 15670 PM* 23 54 40.2073116552 -37 37 40.524416508   10.55 9.76     G8 32 0
15 CD-38 15670b Pl 23 54 40.2073116552 -37 37 40.524416508           ~ 39 0

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