2016MNRAS.461..929K


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.20CEST14:59:26

2016MNRAS.461..929K - Mon. Not. R. Astron. Soc., 461, 929-938 (2016/September-1)

Search for exoplanets and brown dwarfs with VLBI.

KATARZYNSKI K., GAWRONSKI M. and GOZDZIEWSKI K.

Abstract (from CDS):

The main aim of this work is to estimate possible radio GHz emission of extrasolar planets and brown dwarfs and to check if such radiation can be detected by Very Large Baseline Interferometers (VLBI). In the estimation we assume that the emission may originate in processes similar to those observed in the Jupiter system. The frequency of the radio emission that is produced in this system depends mostly on the magnetic field strength. Jupiter's magnetic field (∼9 G on average) allows for radiation from kHz frequencies up to 40 MHz. This is well below the frequency range of VLBI. However, it was demonstrated that the magnetic field strength in massive and young object may be up to two orders of magnitude higher than for Jupiter, which is especially relevant for planets around short-lived A type stars. This should extend the range of the emission up to GHz frequencies. We calculated expected flux densities of radio emission for a variety of hypothetical young planetary systems. We analysed two different emission scenarios, and found that the radiation induced by moons (process similar to Jupiter-Io interactions) appears to be less efficient than the emission generated by a stellar wind on a planetary magnetosphere. We also estimated hypothetical emission of planets and brown dwarfs located around relatively young and massive main-sequence A-type stars. Our results show that the emission produced by stellar winds could be detected by currently operating VLBI networks.

Abstract Copyright: © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): planets and satellites: detection - planets and satellites: magnetic fields - planets and satellites: physical evolution - planet-star interactions - planetary systems - planetary systems

Simbad objects: 47

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Number of rows : 47

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 1160 * 00 15 57.3020078544 +04 15 04.004951787   7.159 7.119     A0V 73 1
2 HD 1237b Pl 00 16 12.67797 -79 51 04.2427           ~ 52 1
3 HD 13445b Pl 02 10 25.9475 -50 49 25.522           ~ 89 1
4 HD 15082b Pl 02 26 51.0582746497 +37 33 01.737746137           ~ 155 1
5 * gam Cet ** 02 43 18.03910 +03 14 08.9390 3.63 3.56 3.47 3.36 3.32 A2Vn+F4V 167 0
6 * tau03 Eri PM* 03 02 23.4993908 -23 37 28.093588 4.33 4.25 4.09 3.96 3.87 A3IV-V 147 0
7 * eps Eri b Pl 03 32 55.84496 -09 27 29.7312           ~ 102 1
8 * bet Eri PM* 05 07 50.98549 -05 05 11.2055 3.02 2.92 2.79 2.65 2.57 A3IV 207 0
9 * zet Lep * 05 46 57.3409587 -14 49 19.019943   3.637 3.525     A2IV-V(n) 277 0
10 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1597 1
11 * bet Pic b Pl 05 47 17.0919798264 -51 03 59.412857187           ~ 305 1
12 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A1V+DA 1373 0
13 * q Pup PM* 08 18 33.3129914 -36 39 33.439105 4.75 4.68 4.40 4.24 4.11 A8V 80 0
14 * 21 LMi dS* 10 07 25.7629578 +35 14 40.896470 4.74 4.67 4.49 4.31 4.24 A7V(n) 212 0
15 2MASSW J1047539+212423 BD* 10 47 53.85 +21 24 23.5           T6.5 69 0
16 HD 95086b Pl 10 57 03.0216129217 -68 40 02.446874288           ~ 64 1
17 * bet UMa PM* 11 01 50.4765370 +56 22 56.733912 2.35 2.35 2.37 2.31 2.35 A1IVps 401 1
18 * del Leo PM* 11 14 06.50142 +20 31 25.3853 2.79 2.68 2.53 2.44 2.41 A5IV(n) 264 0
19 * gam Crt ** 11 24 52.9236199 -17 41 02.429978   4.29 4.08 6.12   A7V(n) 116 1
20 * bet Leo dS* 11 49 03.57834 +14 34 19.4090 2.30 2.22 2.13 2.08 2.06 A3Va 533 0
21 * gam UMa Em* 11 53 49.8473166 +53 41 41.135025 2.440 2.450 2.440 2.44 2.47 A0Ve+K2V 376 0
22 * del UMa PM* 12 15 25.5606327 +57 01 57.415606 3.460 3.410 3.320 3.25 3.25 A2Vn 278 0
23 * del Crv PM* 12 29 51.8551642 -16 30 55.552542 2.80 2.89 2.94 2.99 3.03 A0IV(n)kB9 182 0
24 * eps UMa a2* 12 54 01.7495922 +55 57 35.362645 1.76 1.75 1.77 1.79 1.82 A1III-IVpkB9 453 0
25 * zet Vir PM* 13 34 41.5933793869 -00 35 45.009664548 3.58 3.50 3.38 3.31 3.25 A2Van 179 0
26 * tau Boo b Pl 13 47 15.74340 +17 27 24.8552           ~ 228 1
27 * iot Boo dS* 14 16 09.9303389767 +51 22 02.032771982 5.01 4.95 4.75 4.60 4.51 A7V 151 1
28 * alf Cir a2* 14 42 30.4195804 -64 58 30.493451 3.55 3.43 3.19 2.96 2.86 A7VpSrCrEu 326 0
29 TVLM 513-46 BD* 15 01 08.1871800643 +22 50 02.120480463   21.4 15.09 18.0   M8.5V 145 0
30 HD 133803 gD* 15 07 14.9365807309 -29 30 16.135802450   8.47 8.12     F2IVm-2 41 0
31 HD 145689 PM* 16 17 05.4100392664 -67 56 28.624694971   6.090 5.944     A3V 51 0
32 * 72 Oph PM* 18 07 20.9839294 +09 33 49.850100 3.95 3.85 3.73 3.59 3.54 A5V 130 0
33 CD-29 14904B *i* 18 24 29.2 -29 46 47     14.0     ~ 1 0
34 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2472 0
35 * zet Aql PM* 19 05 24.6080155 +13 51 48.518212 2.99 3.00 2.99 2.98 2.98 A0IV-Vnn 317 0
36 * 59 Dra PM* 19 09 09.8793494721 +76 33 37.808283506   5.400 5.107     A7V 112 1
37 * alf Aql dS* 19 50 46.99855 +08 52 05.9563 1.07 0.98 0.76 0.62 0.49 A7Vn 805 0
38 * eta Ind dS* 20 44 02.3340423 -51 55 15.496981   4.767 4.495     A9IV 75 0
39 * alf Cep PM* 21 18 34.77233 +62 35 08.0681 2.770 2.680 2.460 2.22 2.11 A8Vn 339 0
40 * tet Peg PM* 22 10 11.9852752 +06 11 52.307750 3.72 3.62 3.55 3.50 3.46 A1Va 161 0
41 BD-15 6290b Pl 22 53 16.73352 -14 15 49.3186           ~ 216 1
42 * alf PsA b Pl 22 57 39.04625 -29 37 20.0533           ~ 176 1
43 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1099 3
44 HD 218396e Pl 23 07 28.7156905667 +21 08 03.302133882           ~ 108 1
45 HD 218396d Pl 23 07 28.7156905667 +21 08 03.302133882           ~ 156 1
46 HD 218396c Pl 23 07 28.7156905667 +21 08 03.302133882           ~ 172 1
47 HD 218396b Pl 23 07 28.7156905667 +21 08 03.302133882           ~ 184 1

    Equat.    Gal    SGal    Ecl

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2019.10.20-14:59:26

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