2016A&A...594A..95A


Query : 2016A&A...594A..95A

2016A&A...594A..95A - Astronomy and Astrophysics, volume 594A, 95-95 (2016/10-1)

Simulating the environment around planet-hosting stars. II. Stellar winds and inner astrospheres.

ALVARADO-GOMEZ J.D., HUSSAIN G.A.J., COHEN O., DRAKE J.J., GARRAFFO C., GRUNHUT J. and GOMBOSI T.I.

Abstract (from CDS):

We present the results of a comprehensive numerical simulation of the environment around three exoplanet-host stars (HD 1237, HD 22049, and HD 147513). Our simulations consider one of the latest models currently used for space weather studies in the Heliosphere, with turbulent Alfven wave dissipation as the source of coronal heating and stellar wind acceleration. Large-scale magnetic field maps, recovered with two implementations of the tomographic technique of Zeeman-Doppler imaging, serve to drive steady-state solutions in each system. This paper contains the description of the stellar wind and inner astrosphere, while the coronal structure was discussed in a previous paper. The analysis includes the magneto-hydrodynamical properties of the stellar wind, the associated mass and angular momentum loss rates, as well as the topology of the astrospheric current sheet in each system. A systematic comparison among the considered cases is performed, including two reference solar simulations covering activity minimum and maximum. For HD 1237, we investigate the interactions between the structure of the developed stellar wind, and a possible magnetosphere around the Jupiter-mass planet in this system. We find that the process of particle injection into the planetary atmosphere is dominated by the density distribution rather than the velocity profile of the stellar wind. In this context, we predict a maximum exoplanetary radio emission of 12mJy at 40MHz in this system, assuming the crossing of a high-density streamer during periastron passage. Furthermore, in combination with the analysis performed in the first paper of this study, we obtain for the first time a fully simulated mass loss-activity relation. This relation is compared and discussed in the context of the previously proposed observational counterpart, derived from astrospheric detections. Finally, we provide a characterisation of the global 3D properties of the stellar wind of these systems, at the inner edges of their habitable zones.

Abstract Copyright: © ESO, 2016

Journal keyword(s): stars: winds, outflows - stars: mass-loss - stars: magnetic field - stars: late-type - magnetohydrodynamics (MHD)

Simbad objects: 15

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Number of rows : 15
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 HD 1237 PM* 00 16 12.6791488703 -79 51 04.244738563 7.692 7.335 6.578     G8V 209 1
2 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1769 1
3 HD 22040 * 03 34 04.3930695651 +24 18 31.348466839   9.36 9.24     A0 7 0
4 HD 22029 * 03 36 10.9055570174 +60 34 40.357540851   9.98 9.57     A5 3 0
5 * pi.01 UMa BY* 08 39 11.7043265307 +65 01 15.268273190 6.33 6.26 5.64 5.12 4.79 G0.5V 533 0
6 * 61 Vir PM* 13 18 24.3142756 -18 18 40.304648 5.710 5.440 4.740     G6.5V 619 1
7 NAME Proxima Centauri Er* 14 29 42.9451234609 -62 40 46.170818907 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1093 0
8 * alf Cen ** 14 39 29.71993 -60 49 55.9990   0.4 -0.1     G2V+K1V 874 0
9 * ksi Boo BY* 14 51 23.37993 +19 06 01.6994 5.618 5.370 4.593 3.91 3.48 G7Ve+K5Ve 444 0
10 HD 147513 PM* 16 24 01.2905970257 -39 11 34.734611237 6.17 6.02 5.376     G5V 322 1
11 * 36 Oph ** 17 15 20.9839376 -26 36 10.157115           K2V+K1V 122 0
12 * 70 Oph Ro* 18 05 27.28518 +02 30 00.3558 5.40 4.89 4.03 3.38 2.92 K0-V 617 0
13 * 61 Cyg ** 21 06 53.95 +38 44 57.9           ~ 164 0
14 * eps Ind PM* 22 03 21.6542294981 -56 47 09.537018193   5.75 4.69     K5V 499 0
15 V* EV Lac Er* 22 46 49.7311740821 +44 20 02.372223230   11.85 10.26 9.89   M4.0V 832 2

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2021.12.07-07:31:13

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