2015ApJ...812L..35F


Query : 2015ApJ...812L..35F

2015ApJ...812L..35F - Astrophys. J., 812, L35 (2015/October-3)

A bimodal correlation between host star chromospheric emission and the surface gravity of hot jupiters.

FOSSATI L., INGRASSIA S. and LANZA A.F.

Abstract (from CDS):

The chromospheric activity index of stars hosting transiting hot Jupiters appears to be correlated with the planets' surface gravity. One of the possible explanations is based on the presence of condensations of planetary evaporated material located in a circumstellar cloud that absorbs the Ca ii H&K and Mg ii h&k resonance line emission flux, used to measure chromospheric activity. A larger column density in the condensations, or equivalently a stronger absorption in the chromospheric lines, is obtained when the evaporation rate of the planet is larger, which occurs for a lower gravity of the planet. We analyze here a sample of stars hosting transiting hot Jupiters tuned in order to minimize systematic effects (e.g., interstellar medium absorption). Using a mixture model, we find that the data are best fit by a two-linear-regression model. We interpret this result in terms of the Vaughan-Preston gap. We use a Monte Carlo approach to best take into account the uncertainties, finding that the two intercepts fit the observed peaks of the distribution of for main-sequence solar-like stars. We also find that the intercepts are correlated with the slopes, as predicted by the model based on the condensations of planetary evaporated material. Our findings bring further support to this model, although we cannot firmly exclude different explanations. A precise determination of the slopes of the two linear components would allow one to estimate the average effective stellar flux powering planetary evaporation, which can then be used for theoretical population and evolution studies of close-in planets.

Abstract Copyright:

Journal keyword(s): planet-star interactions - stars: activity - stars: late-type

Simbad objects: 42

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Number of rows : 42
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 WASP-26 * 00 18 24.7008060816 -15 16 02.275778784   11.62 11.30 10.99 10.46 G0 41 1
2 HAT-P-16 * 00 38 17.5584024024 +42 27 47.216738232   11.38 10.91     F8 54 1
3 CD-50 714 PM* 02 27 06.0975766704 -50 17 04.310799828   10.74 10.14     ~ 31 0
4 WASP-50 * 02 54 45.1341750384 -10 53 53.025224640   12.43 11.44 11.599   G9V 35 1
5 WASP-11 ** 03 09 28.5433589520 +30 40 24.862993356   12.58 11.57 11.42   K3V 74 1
6 WASP-22 * 03 31 16.3267124400 -23 49 10.840600632   12.38 11.99 11.41   G 48 1
7 WASP-12 ** 06 30 32.7966092352 +29 40 20.263502460   12.14 11.57     G0V 269 2
8 WASP-23 PM* 06 44 30.6133625784 -42 45 42.666796404   13.42 12.52 12.31   ~ 34 1
9 BD+50 1471 PM* 07 48 06.4723053776 +50 13 32.920598923   12.002 11.138 10.669 10.243 G9V 153 1
10 HAT-P-13 * 08 39 31.8072358440 +47 21 07.273799280   11.15 10.42 10.40   G4 123 2
11 BD+02 2056 * 08 44 25.7031511896 +01 51 36.105474888   11.64 10.83     ~ 19 0
12 BD+34 1976 V* 09 20 24.7145388600 +33 52 56.696039796   11.21 10.42     G1V 60 1
13 WASP-19 V* 09 53 40.0765648584 -45 39 33.057187596   13.05 12.31 12.12 11.35 G8V 156 2
14 CD-29 9873 * 12 42 28.4949559632 -30 38 23.529045948   12.36 11.63 11.39 10.78 G8V 49 1
15 WASP-42 PM* 12 51 55.5581398320 -42 04 25.096306584           ~ 23 1
16 HAT-P-3 * 13 44 22.5937349736 +48 01 43.205733624   12.53 11.86     K1V 73 1
17 HAT-P-12 PM* 13 57 33.4668726399 +43 29 36.601508739   12.6 12.84     K5 69 1
18 HAT-P-44 * 14 12 34.5714083256 +47 00 53.044781616   13.2 13.21 12.83 12.31 ~ 18 1
19 WASP-16 * 14 18 43.9225013904 -20 16 31.843626168   12.51 11.29 11.00 10.49 G3V 60 1
20 HAT-P-27 * 14 51 04.1870399712 +05 56 50.548526376   13.18 12.19 11.98 11.23 G8 51 1
21 BD+36 2593 * 15 19 57.9203617176 +36 13 46.738078788   11.83 11.12     F 95 1
22 BD+28 2507 V* 16 02 11.8462322592 +28 10 10.420201452   11.88 11.25     G1V 96 1
23 HD 149026 PM* 16 30 29.6185771608 +38 20 50.308980864   8.75 8.14     G0IV 211 1
24 1SWASP J175207.01+373246.3 V* 17 52 07.0184259768 +37 32 46.237377840   13.114 12.402 12.06 11.603 G 65 1
25 HAT-P-31 * 18 06 09.0498478464 +26 25 35.989962204   12.02 11.67 11.49   ~ 23 2
26 HAT-P-5 * 18 17 37.3126923960 +36 37 17.170401468   12.92 11.95     G1V 58 1
27 WASP-58 PM* 18 18 48.2529552984 +45 10 19.260291288   12.33 11.66     G2V 24 1
28 V* V672 Lyr V* 19 04 09.8515616256 +36 37 57.446680296   12.35 11.42     K0V 103 1
29 Kepler-1 Er* 19 07 14.0375836512 +49 18 59.091482160   11.85 11.25     G0V 160 2
30 WASP-48 * 19 24 38.9614451424 +55 28 23.332107108   12.31 11.65 11.61   ~ 39 1
31 CoRoT-2 * 19 27 06.4944378024 +01 23 01.359897468   13.422 12.568 12.204 11.49 G7V+K9V 229 2
32 HD 189733 BY* 20 00 43.7129433648 +22 42 39.073143456 9.241 8.578 7.648 7.126 6.68 K2V 805 1
33 WASP-2 V* 20 30 54.1282355304 +06 25 46.341284844   13 11.98     K1.5 124 1
34 BD-05 5432 PM* 21 00 06.1968214728 -05 05 40.034944176   10.93 9.87     ~ 41 1
35 HD 358155 ** 21 01 54.480000 -13 25 59.71008   11.75 10.79 11.12   G4+K3 21 1
36 HAT-P-17 PM* 21 38 08.7310010424 +30 29 19.446386748   11.33 10.38 10.24   G0 48 1
37 HD 209458 V* 22 03 10.7727465312 +18 53 03.549393384   8.21 7.63     F9V 1046 1
38 BD+37 4734B PM* 22 57 46.8442481880 +38 40 30.358351704   10.82 9.87     G0V 150 1
39 WASP-52 * 23 13 58.7576098848 +08 45 40.572305352   12.9 12.0 12.03   K2V 60 1
40 WASP-59 * 23 18 29.5474746528 +24 53 21.438581712   14.01 12.78 12.37   K5V 15 1
41 WASP-4 PM* 23 34 15.0857248317 -42 03 41.047972591   13.51 12.48 11.9   G7V 149 1
42 WASP-5 V* 23 57 23.7564672192 -41 16 37.743700800   12.808 12.146 12.058 11.44 G4V 104 1

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2022.07.06-10:05:21

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