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


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.25CET05:41:29

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 - 2020
#notes
1 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1670 1
2 ICRF J074110.7+311200 Sy1 07 41 10.7033434 +31 12 00.231016   17.02 16.89 16.322   ~ 405 1
3 * bet Gem PM* 07 45 18.94987 +28 01 34.3160 3.00 2.14 1.14 0.39 -0.11 K0IIIb 1042 1
4 ICRF J074640.4+273459 QSO 07 46 40.43230698 +27 34 59.0473025       21.14   ~ 27 1
5 3C 196 Sy1 08 13 36.056090 +48 13 02.63597   18.36 17.79     ~ 473 2
6 3C 295 Sy2 14 11 20.467 +52 12 09.52   22.34 20.80 18.54   ~ 884 5
7 HD 128311 BY* 14 36 00.5607343227 +09 44 47.453643485 9.232 8.441 7.446 6.895 6.425 K3V 264 1
8 ICRF J144828.7+760111 QSO 14 48 28.77904214 +76 01 11.5972889   20.0   21.40   ~ 43 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 298 1
10 * iot Dra V* 15 24 55.7746265 +58 57 57.834445 5.68 4.45 3.29 2.51 1.91 K2III 367 1
11 7C 1603+5722 QSO 16 04 37.3539901706 +57 14 36.667627241   18.02 17.79 17.70   ~ 71 1

    Equat.    Gal    SGal    Ecl

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2020.01.25-05:41:29

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