2019A&A...630A..52R


Query : 2019A&A...630A..52R

2019A&A...630A..52R - Astronomy and Astrophysics, volume 630A, 52-52 (2019/10-1)

Erosion of an exoplanetary atmosphere caused by stellar winds.

RODRIGUEZ-MOZOS J.M. and MOYA A.

Abstract (from CDS):


Aims. We present a formalism for a first-order estimation of the magnetosphere radius of exoplanets orbiting stars in the range from 0.08 to 1.3 M. With this radius, we estimate the atmospheric surface that is not protected from stellar winds. We have analyzed this unprotected surface for the most extreme environment for exoplanets: GKM-type and very low-mass stars at the two limits of the habitable zone. The estimated unprotected surface makes it possible to define a likelihood for an exoplanet to retain its atmosphere. This function can be incorporated into the new habitability index SEPHI.
Methods. Using different formulations in the literature in addition to stellar and exoplanet physical characteristics, we estimated the stellar magnetic induction, the main characteristics of the stellar wind, and the different star-planet interaction regions (sub- and super-Alfvenic, sub- and supersonic). With this information, we can estimate the radius of the exoplanet magnetopause and thus the exoplanet unprotected surface.
Results. We have conducted a study of the auroral aperture angles for Earth-like exoplanets orbiting the habitable zone of its star, and found different behaviors depending on whether the star is in rotational saturated or unsaturated regimes, with angles of aperture of the auroral ring above or below 36°, respectively, and with different slopes for the linear relation between the auroral aperture angle at the inner edge of the habitable zone versus the difference between auroral aperture angles at the two boundaries of the habitable zone. When the planet is tidally locked, the unprotected angle increases dramatically to values higher than 40° with a low likelihood of keeping its atmosphere. When the impact of stellar wind is produced in the sub-Alfvenic regime, the likelihood of keeping the atmosphere is almost zero for exoplanets orbiting very close to their star, regardless of whether they are saturated or not.

Abstract Copyright: © ESO 2019

Journal keyword(s): astrobiology - magnetic fields - planets and satellites: atmospheres - planets and satellites: magnetic fields - stars: magnetic field - planet-star interactions

Simbad objects: 63

goto Full paper

goto View the references in ADS

Number of rows : 63
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 BD+61 195 PM* 01 02 38.8680626986 +62 20 42.175257431   11.439   8.7   M1.5V 230 0
2 NAME YZ Cet b Pl 01 12 30.6367741360 -16 59 56.361313690           ~ 19 0
3 NAME YZ Cet c Pl 01 12 30.6367741360 -16 59 56.361313690           ~ 18 0
4 NAME YZ Cet d Pl 01 12 30.6367741360 -16 59 56.361313690           ~ 16 0
5 V* YZ Cet Er* 01 12 30.6368826382 -16 59 56.358011559 15.315 13.885 12.074 10.696 8.938 M4.0Ve 244 0
6 BD+10 167 PM* 01 20 52.7221427160 +11 27 20.638060092   10.90 10.224     K0 10 0
7 Ross 15 Er* 01 59 23.5137039235 +58 31 16.104337813   12.90 12.155 11.871   M4Ve 87 0
8 NAME Teegarden's Star b Pl 02 53 00.8913291021 +16 52 52.642086267           ~ 12 0
9 NAME Teegarden's Star c Pl 02 53 00.8913291021 +16 52 52.642086267           ~ 15 0
10 NAME Teegarden's Star LM* 02 53 00.8917932409 +16 52 52.632190137   17.21   14.1   dM6 141 0
11 BD-07 699 PM* 03 54 35.4659715007 -06 49 33.654053933 11.693 10.391 9.015 8.167 7.4 K5V 96 0
12 Ross 28 ** 04 12 58.8326322803 +52 36 42.021350887   15.0   13.203   M4.0V 51 0
13 V* V1005 Ori BY* 04 59 34.8342878424 +01 47 00.669818328   11.48 10.107 9.603 8.239 M0Ve 327 0
14 NAME LP 656-38b Pl 05 01 57.4261049715 -06 56 46.371875101           ~ 17 0
15 NAME LP 656-38c Pl 05 01 57.4261049715 -06 56 46.371875101           ~ 13 0
16 LP 656-38 Er* 05 01 57.4261317472 -06 56 46.376281497   13.92 12.196 11.791 9.175 M4.0Ve 126 0
17 BD+43 1596 * 06 46 46.1061839256 +43 35 03.002474724   10.06 8.48     K7III 8 0
18 G 51-15 Er* 08 29 49.3527921926 +26 46 33.624143059   16.87   14.736   M6.5Ve 278 0
19 BD+20 2465 Er* 10 19 36.2808181226 +19 52 12.010446571   10.82 9.52 9.19   dM3 1262 0
20 V* DS Leo BY* 11 02 38.3420210088 +21 58 01.700013360 12.246 11.049 9.572 8.638 7.634 M1.0Ve 209 0
21 BD+44 2051B Er* 11 05 30.8855820790 +43 31 17.885197587   16.45 14.45 13.4   M6.0V 229 0
22 K2-3 PM* 11 29 20.3917077216 -01 27 17.281697868   13.52 12.17 11.88   M1V 64 0
23 K2-3d Pl 11 29 20.3917940095 -01 27 17.279810476           ~ 42 0
24 Ross 128b Pl 11 47 44.3968668170 +00 48 16.404931305           ~ 31 0
25 Ross 128 Er* 11 47 44.3972681420 +00 48 16.400337591 14.223 12.905 11.153 9.859 8.184 dM4 391 0
26 V* GL Vir Er* 12 18 59.3997287457 +11 07 33.773236317   15.68 13.90 13.55   M4.5Ve 160 0
27 BD+13 2618 Er* 13 00 46.5566863405 +12 22 32.677229903 12.314 11.233 9.750 8.785 7.653 M0V 330 1
28 NAME Proxima Centauri b Pl 14 29 42.9451234609 -62 40 46.170818907           ~ 320 0
29 NAME Proxima Centauri Er* 14 29 42.9461331854 -62 40 46.164680672 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1190 0
30 BD+16 2708 Er* 14 54 29.2361840107 +16 06 03.797990080 12.86 11.686 10.150 9.116 7.872 M3V 264 1
31 BD-07 4003 BY* 15 19 26.8269387505 -07 43 20.189497466 13.403 11.76 10.560 9.461 8.911 M3V 601 2
32 BD-07 4003e Pl 15 19 26.8271336166 -07 43 20.190958776           ~ 74 1
33 V* OT Ser PM* 15 21 52.9325510712 +20 58 39.910874376 12.662 11.522 10.003 8.993 7.843 M1.0V 128 0
34 BD-12 4523b Pl 16 30 18.0582010683 -12 39 45.323235188           ~ 19 0
35 BD-12 4523 BY* 16 30 18.0583947383 -12 39 45.321217732 12.829 11.638 10.072 8.917 7.421 M3V 294 0
36 NAME Barnard's star BY* 17 57 48.4984700685 +04 41 36.113879676 12.497 11.24 9.511 8.298 6.741 M4V 764 2
37 GJ 699 b Pl? 17 57 48.4997994034 +04 41 36.111354228           ~ 19 0
38 Kepler-62 Ro* 18 52 51.0518497680 +45 20 59.399622996   14.4 13.8     G5 112 1
39 Kepler-62f Pl 18 52 51.0518996853 +45 20 59.400075457           ~ 68 1
40 Kepler-62e Pl 18 52 51.0518996853 +45 20 59.400075457           ~ 62 1
41 Kepler-442 Ro* 19 01 27.9742961064 +39 16 48.224136216           ~ 29 0
42 Kepler-442b Pl 19 01 27.9742963430 +39 16 48.223608589           ~ 37 0
43 Kepler-1185 EB* 19 08 57.8786105808 +39 19 57.933753168           ~ 38 0
44 Kepler-1185b Pl 19 08 57.8787205167 +39 19 57.934427169           ~ 9 0
45 Kepler-22 PM* 19 16 52.1902276920 +47 53 03.948648180   11.5   11.70   G5 83 1
46 Kepler-22b Pl 19 16 52.1904191915 +47 53 03.947532134           ~ 82 1
47 Kepler-1649 PM* 19 30 00.9006032400 +41 49 49.518349032   19.1   16.6   M5V 27 0
48 Kepler-1649b Pl 19 30 00.9006122986 +41 49 49.513849537           ~ 22 0
49 KOI-2418.01 Pl 19 49 56.8075700263 +46 59 48.107320261           ~ 39 0
50 Kepler-1229 Ro* 19 49 56.8076265768 +46 59 48.103495728           ~ 43 0
51 G 208-45 Er* 19 53 55.1405033909 +44 24 54.147256052   15.97 13.99 14.3 10.27 M6V 179 0
52 Kepler-186 Ro* 19 54 36.6535147488 +43 57 18.025920324           M1V 115 0
53 Kepler-186f Pl 19 54 36.6536205214 +43 57 18.025893926           ~ 73 0
54 V* V374 Peg Er* 22 01 13.1241989539 +28 18 24.907312662       11.602   M3.5Ve 208 0
55 V* EV Lac Er* 22 46 49.7312610268 +44 20 02.374381562   11.85 10.26 9.89   M4.0Ve 865 2
56 TRAPPIST-1d Pl 23 06 29.3684052886 -05 02 29.031690445           ~ 176 0
57 TRAPPIST-1g Pl 23 06 29.3684052886 -05 02 29.031690445           ~ 156 0
58 TRAPPIST-1c Pl 23 06 29.3684052886 -05 02 29.031690445           ~ 149 0
59 TRAPPIST-1e Pl 23 06 29.3684052886 -05 02 29.031690445           ~ 217 0
60 TRAPPIST-1h Pl 23 06 29.3684052886 -05 02 29.031690445           ~ 101 0
61 TRAPPIST-1 LM* 23 06 29.3684948589 -05 02 29.037301866     18.798 16.466 14.024 M7.5e 810 0
62 BD+19 5116A Er* 23 31 52.1738511880 +19 56 14.130398245   12.27 10.173 9.946   M3.5Ve 90 0
63 BD+19 5116B Er* 23 31 52.5753377942 +19 56 14.005026315   14.8   12.165   M4.0Ve 195 0

To bookmark this query, right click on this link: simbad:objects in 2019A&A...630A..52R and select 'bookmark this link' or equivalent in the popup menu


2023.01.30-06:36:14

© Université de Strasbourg/CNRS

    • Contact