SIMBAD references

2012A&A...546A.116S - Astronomy and Astrophysics, volume 546A, 116-116 (2012/10-1)

A stringent upper limit to 18 cm radio emission from the extrasolar planet system τ Bootis.

STROE A., SNELLEN I.A.G. and ROETTGERING H.J.A.

Abstract (from CDS):

It has been speculated for many years that some extrasolar planets may emit strong cyclotron emission at low radio frequencies in the range 10-100MHz. Despite several attempts no such emission has yet been seen. The hot Jupiter system τ Bootis is one of the nearest (d=15pc) exoplanets known to date. The gravitational influence of this massive hot Jupiter (M=6Mjup) has locked the star-planet system, making the star rotate in P∼3.3days, similar to the orbital period of the planet. From the well established correlation between stellar rotation and radio luminosity, it is conceivable that the τ Bootis system emits strong radio emission at significantly higher frequencies than currently probed, which we aimed to investigate with this work. We observed τ Bootis with the Westerbork Synthesis Radio Telescope (WSRT) at a frequency of 1.7GHz. for 12h in spectral line mode, reaching a noise level of 42µJy/beam at the position of the target. No 18cm radio emission is detected from τ Bootis, resulting in a 3σ upper limit of 0.13mJy, corresponding to a 18cm radio luminosity of <3.7x1013erg/s/Hz. We observe τ Bootis to be two orders of magnitude fainter than expected from the stellar relation between radio luminosity and rotation velocity. This implies that either the τ Bootis system is underluminous in the radio compared to similar fast-rotating stars, or that we happened to observe the target during a low state of radio emission.

Abstract Copyright:

Journal keyword(s): planetary systems - radio continuum: stars

Simbad objects: 2

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2012A&A...546A.116S and select 'bookmark this link' or equivalent in the popup menu


2019.10.21-01:04:34

© Université de Strasbourg/CNRS

    • Contact