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).

Abstract Copyright: ©

Journal keyword(s):

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

Simbad objects: 15

Full paper

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Number of rows : 15

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag B	Mag V	Mag R	Mag I	Sp type	#ref 1850 - 2026	#notes
1	HD 3167b	Pl	00 34 57.5242131960	+04 22 53.284093032					~	86	0
2	K2-106b	Pl	00 52 19.1415736296	+10 47 40.906374828					~	67	0
3	HD 10069b	Pl	01 37 25.0332798696	-45 40 40.374717456					~	444	1
4	NGTS-4b	Pl	05 58 23.7549496011	-30 48 42.363268864					~	47	0
5	CoRoT-7b	Pl	06 43 49.4690164104	-01 03 46.826642700					~	422	1
6	* rho01 Cnc e	Pl	08 52 35.8111044043	+28 19 50.954994470					~	682	1
7	WASP-43	PM*	10 19 38.0088913464	-09 48 22.605801336	13.782	12.490	12.022	11.10	K7V	182	1
8	K2-131b	Pl	12 11 00.3783875832	-09 45 54.781040484					~	35	0
9	BD-05 3504b	Pl	12 27 29.5846968120	-06 43 18.766944228					~	58	0
10	Kepler-10b	Pl	19 02 43.0613892904	+50 14 28.701617339					~	322	1
11	Kepler-78b	Pl	19 34 58.0137407208	+44 26 53.960186940					~	153	1
12	WASP-47e	Pl	22 04 48.7261549272	-12 01 07.998743676					~	98	0
13	K2-141b	Pl	23 23 39.9709098120	-01 11 21.448681332					~	104	0
14	CD-38 15670	PM*	23 54 40.2073116552	-37 37 40.524416508	10.55	9.76			G7V	61	0
15	CD-38 15670b	Pl	23 54 40.2073116552	-37 37 40.524416508					~	79	0

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