2014A&A...570A..50S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.11CEST21:12:30

2014A&A...570A..50S - Astronomy and Astrophysics, volume 570A, 50-50 (2014/10-1)

Effects of X-ray and extreme UV radiation on circumbinary planets.

SANZ-FORCADA J., DESIDERA S. and MICELA G.

Abstract (from CDS):

Several circumbinary planets have recently been discovered. The orbit of a planet around a binary stellar system poses several dynamic constraints. In addition to these constraints, the effects that radiation from the host stars may have on the planet atmospheres must be considered. We here evaluate these effects. Because of the configuration of a close binary system, these stars have a high rotation rate, even for old stars. The fast rotation of close, tidally locked binaries causes a permanent state of high stellar activity and copious XUV radiation. The accumulated effects are stronger than for normal exoplanets around single stars and cause a faster evaporation of their atmospheres. We evaluate the effects that stellar radiation has on the evaporation of exoplanets around binary systems and on the survival of these planets. We considered the X-ray and EUV spectral ranges (XUV, 1-912Å) to account for the photons that are easily absorbed by a planet atmosphere that is mainly composed of hydrogen. A more complex atmospheric composition is expected to absorb this radiation more efficiently. We used direct X-ray observations to evaluate the energy in the X-rays range and coronal models to calculate the (nondetectable) EUV part of the spectrum. We considered in this problem different configurations of stellar masses, and a resonance of 4:1 and 3:1. The simulations show that exoplanets orbiting close binary systems in a close orbit will suffer strong photoevaporation that may cause a total loss of atmosphere in a short time. We also applied our models to the best real example, Kepler-47 b, to estimate the current mass-loss rates in circumbinary planets and the accumulated effects over the time. A binary system of two solar-like stars will be highly efficient in evaporating the atmosphere of the planet (less than 6Gyr in our case). These systems will be difficult to find, even if they are dynamically stable. Still, planets may orbit around binary systems of low mass stars for wider orbits. Currently known circumbinary planets are not substantially affected by thermal photoevaporation processes, unless Kepler-47 b has an inflated atmosphere. The distribution of the orbital periods of circumbinary planets is shifted to much longer periods than the average of Kepler planets, which supports a scenario of strong photoevaporation in close-in circumbinary planets.

Abstract Copyright:

Journal keyword(s): planet-star interactions - planetary systems - binaries (including multiple): close - stars: coronae - X-rays: stars - stars: individual: Kepler-47

Simbad objects: 26

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Number of rows : 26

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 SCR J0103-5515C LM* 01 03 35.58 -55 15 54.6           ~ 30 0
2 HD 13445b Pl 02 10 25.9190575041 -50 49 25.467227759           ~ 90 1
3 V* UZ For AM* 03 35 28.6515678221 -25 44 21.765602833           M4.5 245 0
4 V* RR Cae WD* 04 21 05.5631969817 -48 39 07.062891386 14.50 14.92 14.40     DA7.8 134 1
5 V* FW Tau Or* 04 29 29.703744 +26 16 53.06412       15.85   M5.5 116 0
6 V* DP Leo AM* 11 17 15.9238061197 +17 57 41.680410866           ~ 210 1
7 BD-07 3477 HS* 12 44 20.2386520980 -08 40 16.848587212   10.46 10.594 10.895   sdB2VIIHe3 249 1
8 ULAS J130041.74+122114.7 BD* 13 00 42.08415 +12 21 15.0536         23.28 T8.5p 100 0
9 V* NY Vir HS* 13 38 48.1466489725 -02 01 49.209465866   13.43 13.66 13.75   sdB1VIIHe1 191 1
10 V* NN Ser No* 15 52 56.1202658103 +12 54 44.432043501     16.51     DAO1+M4 232 0
11 PSR B1620-26 Psr 16 23 38.2218 -26 31 53.769     21.30     ~ 269 2
12 NAME SR 12C LM* 16 27 19.66704 -24 41 48.8292           M9.0 30 0
13 ROXs 42B TT* 16 31 15.0191785687 -24 32 43.717222006     14.27 13.03 11.72 ~ 44 0
14 Kepler-38b Pl 19 07 19.2813795966 +42 16 45.120332899           ~ 46 1
15 Kepler-413b Pl 19 14 02.5618062386 +51 09 45.019125804           ~ 40 0
16 Kepler-16b Pl 19 16 18.1759181246 +51 45 26.777781114           ~ 109 1
17 Kepler-42c Pl 19 28 52.5687991194 +44 37 08.990276298           ~ 39 1
18 Kepler-35b Pl 19 37 59.2726236478 +46 41 22.952068619           ~ 75 1
19 Kepler-47c Pl 19 41 11.4984891255 +46 55 13.705101341           ~ 50 1
20 Kepler-47b Pl 19 41 11.4984891255 +46 55 13.705101341           ~ 56 1
21 Kepler-47 Al* 19 41 11.4984891255 +46 55 13.705101341           ~ 122 1
22 Kepler-34b Pl 19 45 44.5975310719 +44 38 29.612454271           ~ 81 1
23 Kepler-64b Pl 19 52 51.6169691968 +39 57 18.370395541           ~ 43 1
24 HD 189733b Pl 20 00 43.7130382888 +22 42 39.071811263           ~ 1082 1
25 HD 189733 BY* 20 00 43.7130382888 +22 42 39.071811263 9.241 8.578 7.648 7.126 6.68 K2V 720 1
26 V* HU Aqr AM* 21 07 58.1945403160 -05 17 40.557984218   15.1   15.4   D+M4V 256 1

    Equat.    Gal    SGal    Ecl

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2020.07.11-21:12:30

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