2016A&A...586A..75S


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.18CEST14:34:13

2016A&A...586A..75S - Astronomy and Astrophysics, volume 586A, 75-75 (2016/2-1)

Simulating the escaping atmospheres of hot gas planets in the solar neighborhood.

SALZ M., CZESLA S., SCHNEIDER P.C. and SCHMITT J.H.M.M.

Abstract (from CDS):

Absorption of high-energy radiation in planetary thermospheres is generally believed to lead to the formation of planetary winds. The resulting mass-loss rates can affect the evolution, particularly of small gas planets. We present 1D, spherically symmetric hydrodynamic simulations of the escaping atmospheres of 18 hot gas planets in the solar neighborhood. Our sample only includes strongly irradiated planets, whose expanded atmospheres may be detectable via transit spectroscopy using current instrumentation. The simulations were performed with the PLUTO-CLOUDY interface, which couples a detailed photoionization and plasma simulation code with a general MHD code. We study the thermospheric escape and derive improved estimates for the planetary mass-loss rates. Our simulations reproduce the temperature-pressure profile measured via sodium D absorption in HD189733b, but show still unexplained differences in the case of HD209458b. In contrast to general assumptions, we find that the gravitationally more tightly bound thermospheres of massive and compact planets, such as HAT-P-2b are hydrodynamically stable. Compact planets dispose of the radiative energy input through hydrogen Lyα and free-free emission. Radiative cooling is also important in HD189733b, but it decreases toward smaller planets like GJ436b. Computing the planetary Lyα absorption and emission signals from the simulations, we find that the strong and cool winds of smaller planets mainly cause strong Lyα absorption but little emission. Compact and massive planets with hot, stable thermospheres cause small absorption signals but are strong Lyα emitters, possibly detectable with the current instrumentation. The absorption and emission signals provide a possible distinction between these two classes of thermospheres in hot gas planets. According to our results, WASP-80 and GJ 3470 are currently the most promising targets for observational follow-up aimed at detecting atmospheric Lyα absorption signals.

Abstract Copyright:

Journal keyword(s): methods: numerical - hydrodynamics - radiation mechanisms: non-thermal - planets and satellites: atmospheres - planets and satellites: dynamical evolution and stability

VizieR on-line data: <Available at CDS (J/A+A/586/A75): stars.dat 55cncb.dat corot2b.dat gj1214b.dat gj3470b.dat gj436b.dat hatp11b.dat hd149026.dat hd189733.dat hd209458.dat hd97658b.dat wasp10b.dat wasp12b.dat wasp43b.dat wasp77b.dat wasp80b.dat wasp8b.dat>

Simbad objects: 46

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Number of rows : 46

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 HD 10069 * 01 37 25.0335097438 -45 40 40.376513381   9.74 9.30     F6IV/V 139 1
2 WASP-18b Pl 01 37 25.0335097438 -45 40 40.376513381           ~ 187 1
3 BD-07 436 ** 02 28 37.226 -07 03 38.39   10.87 10.12 10.23   ~ 15 0
4 WASP-77Ab Pl 02 28 37.2275829401 -07 03 38.378689023           ~ 20 1
5 BD-07 436B PM* 02 28 37.3244185011 -07 03 41.286377282     13.40     K5 8 0
6 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2908 0
7 WASP-12 ** 06 30 32.7966788910 +29 40 20.266334158   12.14 11.57     G0V 208 2
8 WASP-12b Pl 06 30 32.7966788910 +29 40 20.266334158           G0 486 1
9 HAT-P-20 PM* 07 27 39.9487418539 +24 20 11.518276475   12.58 11.35 11.00   K3V 47 1
10 HAT-P-20b Pl 07 27 39.9487418539 +24 20 11.518276475           ~ 50 1
11 LP 424-4 PM* 07 59 05.8395618539 +15 23 29.240025256   13.5   11.934   M2.0Ve 63 1
12 GJ 3470 b Pl 07 59 05.8395618539 +15 23 29.240025256           ~ 125 1
13 * rho01 Cnc b Pl 08 52 35.81093 +28 19 50.9511     13.16     ~ 224 1
14 * rho01 Cnc e Pl 08 52 35.81093 +28 19 50.9511           ~ 355 1
15 * rho01 Cnc PM* 08 52 35.8113282132 +28 19 50.956901366 7.45 6.82   5.4   K0IV-V 945 1
16 WASP-43b Pl 10 19 38.0089444408 -09 48 22.603103969           ~ 171 1
17 WASP-43 PM* 10 19 38.0089444408 -09 48 22.603103969   13.4 12.4 12.08 11.10 K7V 68 1
18 HD 97658 PM* 11 14 33.1613362847 +25 42 37.391912066 9.049 8.569 7.714 7.259 6.835 K1V 121 1
19 HD 97658b Pl 11 14 33.1613362847 +25 42 37.391912066           ~ 121 1
20 Ross 905b Pl 11 42 11.0932 +26 42 23.653           ~ 547 1
21 Ross 905 PM* 11 42 11.0933874353 +26 42 23.658083337   12.06 10.613 10.272 8.24 M3V 471 1
22 HD 146389 * 16 15 50.3652643210 +10 01 57.284401784   9.866 9.39 9.22   F8 39 1
23 WASP-38b Pl 16 15 50.3652643210 +10 01 57.284401784           ~ 35 1
24 HD 147506b Pl 16 20 36.3579144486 +41 02 53.109043943           ~ 205 1
25 HD 147506 * 16 20 36.3579144486 +41 02 53.109043943   9.15 8.69     F8V 135 2
26 HD 149026 PM* 16 30 29.6184841164 +38 20 50.310893575   8.75 8.14     G0IV 192 1
27 HD 149026b Pl 16 30 29.6184841164 +38 20 50.310893575           ~ 288 1
28 G 139-21 PM* 17 15 18.9337265994 +04 57 50.064695682   16.40   14.394   M4.5V 219 1
29 NAME LHS 3275b Pl 17 15 18.94 +04 57 49.7           ~ 488 1
30 CoRoT-2 * 19 27 06.4944821296 +01 23 01.357597206   13.422 12.568 12.204 11.49 G7V+K9V 201 2
31 CoRoT-2b Pl 19 27 06.4944821296 +01 23 01.357597206     12.57     ~ 170 1
32 KOI-680b Pl? 19 29 08.9490750554 +43 11 50.160271524           ~ 6 1
33 KOI-3.01 Pl 19 50 50.2474562793 +48 04 51.097364378           ~ 259 1
34 BD+47 2936 EB* 19 50 50.2474562793 +48 04 51.097364378       8.8   K4V 199 4
35 HD 189733 BY* 20 00 43.7130382888 +22 42 39.071811263 9.241 8.578 7.648 7.126 6.68 K0V+M4V 689 1
36 HD 189733b Pl 20 00 43.7130382888 +22 42 39.071811263           ~ 1005 1
37 WASP-80b Pl 20 12 40.1691752075 -02 08 39.191157456           ~ 48 1
38 WASP-80 * 20 12 40.1691752075 -02 08 39.191157456   12.810 11.939 11.510 10.279 K7V-M0V 33 1
39 V* V376 Peg EP* 22 03 10.7729598762 +18 53 03.548248479   8.21 7.63     F9V 968 1
40 HD 209458b Pl 22 03 10.7729598762 +18 53 03.548248479           ~ 1396 1
41 WASP-10 V* 23 15 58.3005497925 +31 27 46.294728182   12.4   12.03   K5V 73 1
42 WASP-10b Pl 23 15 58.3005497925 +31 27 46.294728182           ~ 84 1
43 WASP-59b Pl 23 18 29.54 +24 53 21.4           ~ 24 1
44 CD-35 16019A PM* 23 59 36.0711854449 -35 01 52.923483315   10.69 9.87     G6 45 0
45 NAME CD-35 16019Ab Pl 23 59 36.0711854449 -35 01 52.923483315           ~ 87 0
46 NAME Local Bubble ISM ~ ~           ~ 661 0

    Equat.    Gal    SGal    Ecl

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2019.10.18-14:34:13

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