2018A&A...612A..52O


Query : 2018A&A...612A..52O

2018A&A...612A..52O - Astronomy and Astrophysics, volume 612A, 52-52 (2018/4-1)

A search for radio emission from exoplanets around evolved stars.

O'GORMAN E., COUGHLAN C.P., VLEMMINGS W., VARENIUS E., SIROTHIA S., RAY T.P. and OLOFSSON H.

Abstract (from CDS):

The majority of searches for radio emission from exoplanets have to date focused on short period planets, i.e., the so-called hot Jupiter type planets. However, these planets are likely to be tidally locked to their host stars and may not generate sufficiently strong magnetic fields to emit electron cyclotron maser emission at the low frequencies used in observations (typically ≥150MHz). In comparison, the large mass-loss rates of evolved stars could enable exoplanets at larger orbital distances to emit detectable radio emission. Here, we first show that the large ionized mass-loss rates of certain evolved stars relative to the solar value could make them detectable with the LOw Frequency ARray (LOFAR) at 150MHz (λ=2m), provided they have surface magnetic field strengths >50G. We then report radio observations of three long period (>1au) planets that orbit the evolved stars β Gem, ι Dra, and β UMi using LOFAR at 150 MHz. We do not detect radio emission from any system but place tight 3σ upper limits of 0.98, 0.87, and 0.57mJy on the flux density at 150 MHz for β Gem, ι Dra, and β UMi, respectively. Despite our non-detections these stringent upper limits highlight the potential of LOFAR as a tool to search for exoplanetary radio emission at meter wavelengths.

Abstract Copyright: © ESO 2018

Journal keyword(s): radio continuum: planetary systems - planets and satellites: detection - planets and satellites: magnetic fields - planets and satellites: aurorae - stars: evolution - surveys

CDS comments: Calibrator JVAS J1527+5849 not identified.

Simbad objects: 11

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Number of rows : 11
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 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 1828 1
2 ICRF J074110.7+311200 Sy1 07 41 10.70330407 +31 12 00.2291151   17.02 16.89 16.322   ~ 432 1
3 * bet Gem PM* 07 45 18.94987 +28 01 34.3160 3.00 2.14 1.14 0.39 -0.11 K0IIIb 1081 1
4 ICRF J074640.4+273459 QSO 07 46 40.43231234 +27 34 59.0470434       21.14   ~ 38 1
5 3C 196 Sy1 08 13 36.0561170112 +48 13 02.644966020   18.36 17.79     ~ 527 2
6 3C 295 Sy2 14 11 20.467 +52 12 09.52   22.34 20.80 18.54   ~ 949 5
7 HD 128311 BY* 14 36 00.5602765558 +09 44 47.454573266 9.232 8.441 7.446 6.895 6.425 K3V 293 1
8 ICRF J144828.7+760111 QSO 14 48 28.77907399 +76 01 11.5972341   20.0   21.40   ~ 44 1
9 * bet UMi V* 14 50 42.32580 +74 09 19.8142 5.32 3.55 2.08 0.97 0.21 K4-III 316 0
10 * iot Dra V* 15 24 55.7746265 +58 57 57.834445 5.68 4.45 3.29 2.51 1.91 K2III 392 1
11 7C 1603+5722 QSO 16 04 37.3548559224 +57 14 36.660126444   18.02 17.79 17.70   ~ 84 1

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2022.12.09-20:19:36

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