Identification

Title

Searching for star-planet interactions in GJ 486 at radio wavelengths with the uGMRT

Abstract

Aims. We search for radio emission from star–planet interactions in the M dwarf system GJ 486, which hosts an Earth-like planet.<p style="-webkit-text-stroke-width:0px;background-color:rgb(255, 255, 255);color:rgb(51, 51, 51);font:400 1.35rem / 1.8rem "Crimson Text", Georgia, "Open Sans", Calibri, Verdana, Arial, sans-serif;letter-spacing:normal;margin:5px 0px 0px;orphans:2;text-align:justify;text-decoration-color:initial;text-decoration-style:initial;text-decoration-thickness:initial;text-indent:0px;text-transform:none;white-space:normal;widows:2;word-spacing:0px;">Methods. We observed the GJ 486 system with the upgraded Giant Metrewave Radio Telescope (uGMRT) from 550 to 750 MHz in nine different epochs between October 2021 and February 2022, covering almost all orbital phases of GJ 486b from different orbital cycles. We obtained radio images and dynamic spectra of the total and circularly polarized intensity for each individual epoch.<p style="-webkit-text-stroke-width:0px;background-color:rgb(255, 255, 255);color:rgb(51, 51, 51);font:400 1.35rem / 1.8rem "Crimson Text", Georgia, "Open Sans", Calibri, Verdana, Arial, sans-serif;letter-spacing:normal;margin:5px 0px 0px;orphans:2;text-align:justify;text-decoration-color:initial;text-decoration-style:initial;text-decoration-thickness:initial;text-indent:0px;text-transform:none;white-space:normal;widows:2;word-spacing:0px;">Results. We did not detect any quiescent radio emission in any epoch above 3σ. Similarly, we did not detect any bursty emission in our dynamic spectra.<p style="-webkit-text-stroke-width:0px;background-color:rgb(255, 255, 255);color:rgb(51, 51, 51);font:400 1.35rem / 1.8rem "Crimson Text", Georgia, "Open Sans", Calibri, Verdana, Arial, sans-serif;letter-spacing:normal;margin:5px 0px 0px;orphans:2;text-align:justify;text-decoration-color:initial;text-decoration-style:initial;text-decoration-thickness:initial;text-indent:0px;text-transform:none;white-space:normal;widows:2;word-spacing:0px;">Conclusions. While we cannot completely rule out that the absence of a radio detection is due to time variability of the radio emission or to the maximum electron-cyclotron maser emission being below our observing range, these cases seem unlikely. We discuss two possible scenarios: an intrinsic dim radio signal and, alternatively, a situation where the anisotropic beamed emission is pointed away from the observer. If the non-detection of radio emission from the star-planet interaction in GJ 486 is due to an intrinsically dim signal, this implies that independent of whether the planet is magnetized or not, the mass-loss rate is small (Ṁ⋆ ≲ 0.3 Ṁ⊙) and that, concomitantly, the efficiency of the conversion of the Poynting flux into radio emission must be low (β ≲ 10−3). Free-free absorption effects are negligible, given the high value of the coronal temperature. Finally, if the anisotropic beaming pointed away from the observer, this would imply that GJ 486 has very low values of magnetic obliquity and inclination.

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document

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https://n2t.net/ark:/85065/d7hq447b

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eng

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geoscientificInformation

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publication

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2016-01-01T00:00:00Z

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publication

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2025-01-01T00:00:00Z

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Copyright author(s). This work is licensed under a Creative Commons Attribution-NonCommercial 4.0 International License.

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OpenSky Support

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UCAR/NCAR - Library

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PO Box 3000

Boulder

80307-3000

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opensky@ucar.edu

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http://opensky.ucar.edu/

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