Emission of cyclotron radiation by interstellar planets

H. Vanhamäki

研究成果: Contribution to journalArticle査読

5 被引用数 (Scopus)

抄録

In the solar system all planets that have significant magnetic fields also emit electron cyclotron radiation, usually near the auroral regions around the magnetic poles. In this study we use scaling laws based on solar system data to estimate the power and frequency of the auroral cyclotron emissions from interstellar planets (or sub-brown dwarfs). The emission can be powered either by motion of the planet through the interstellar plasma or by unipolar induction due to a moon. According to our results, in interstellar space the unipolar induction mechanism is potentially more effective than the motional emission mechanism. Typical emission power is around 10101012 W, but significantly stronger emissions are obtained in the most optimistic estimates. We have to conclude that detection of a rogue Jupiter would be very difficult, if not impossible with the radio telescopes available now or in the near future, but in very favorable conditions a much more massive and rapidly rotating (or otherwise strongly magnetized) gas giant with a large nearby moon could be detected up to ∼57 pc distance with the square kilometer array. There may be a few thousand large enough interstellar planets this close to the solar system. For reference, we point out that according to previous studies some known hot Jupiters are expected to emit up to 101410 16 W of cyclotron radiation, orders of magnitude more than the typical interstellar planets discussed here. However, these emissions have not yet been detected.

本文言語英語
ページ(範囲)862-869
ページ数8
ジャーナルPlanetary and Space Science
59
9
DOI
出版ステータス出版済み - 7 2011
外部発表はい

All Science Journal Classification (ASJC) codes

  • 天文学と天体物理学
  • 宇宙惑星科学

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