Searching for star-planet interactions in GJ 486 at radio wavelengths with the uGMRT
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arXiv
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| Autori principali: | , , , , , , , , , , , , , , , , |
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| Natura: | Preprint |
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2024
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| author | Peña-Moñino, L. Pérez-Torres, M. Kansabanik, D. Blázquez-Calero, G. Kavanagh, R. D. Gómez, J. F. Moldón, J. Alberdi, A. Amado, P. J. Anglada, G. Caballero, J. A. Mohan, A. Leto, P. Narang, M. Osorio, M. Revilla, D. Trigilio, C. |
| author_facet | Peña-Moñino, L. Pérez-Torres, M. Kansabanik, D. Blázquez-Calero, G. Kavanagh, R. D. Gómez, J. F. Moldón, J. Alberdi, A. Amado, P. J. Anglada, G. Caballero, J. A. Mohan, A. Leto, P. Narang, M. Osorio, M. Revilla, D. Trigilio, C. |
| contents | We search for radio emission from star-planet interactions in the M-dwarf system GJ~486, which hosts an Earth-like planet. 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~486 b from different orbital cycles. We obtained radio images and dynamic spectra of the total and circularly polarized intensity for each individual epoch We do not detect any quiescent radio emission in any epoch above 3$σ$. Similarly, we do not detect any bursty emission in our dynamic spectra.
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, this seems unlikely. We discuss two possible scenarios: an intrinsic dim radio signal, or alternatively, that the anisotropic beamed emission pointed away from the observer. If the non-detection of radio emission from star-planet interaction in GJ~486 is due to an intrinsically dim signal, this implies that, independently of whether the planet is magnetized or not, the mass-loss rate is small (\dot{M}_\star $\lesssim$ 0.3 \dot{M}_\sun) and that, concomitantly, the efficiency of the conversion of Poynting flux into radio emission must be low ($β\lesssim 10^{-3}$). Free-free absorption effects are negligible, given the high value of the coronal temperature. Finally, if the anisotropic beaming pointed away from us, this would imply that GJ~486 has very low values of its magnetic obliquity and inclination. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2411_17689 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Searching for star-planet interactions in GJ 486 at radio wavelengths with the uGMRT Peña-Moñino, L. Pérez-Torres, M. Kansabanik, D. Blázquez-Calero, G. Kavanagh, R. D. Gómez, J. F. Moldón, J. Alberdi, A. Amado, P. J. Anglada, G. Caballero, J. A. Mohan, A. Leto, P. Narang, M. Osorio, M. Revilla, D. Trigilio, C. Earth and Planetary Astrophysics Solar and Stellar Astrophysics We search for radio emission from star-planet interactions in the M-dwarf system GJ~486, which hosts an Earth-like planet. 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~486 b from different orbital cycles. We obtained radio images and dynamic spectra of the total and circularly polarized intensity for each individual epoch We do not detect any quiescent radio emission in any epoch above 3$σ$. Similarly, we do not detect any bursty emission in our dynamic spectra. 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, this seems unlikely. We discuss two possible scenarios: an intrinsic dim radio signal, or alternatively, that the anisotropic beamed emission pointed away from the observer. If the non-detection of radio emission from star-planet interaction in GJ~486 is due to an intrinsically dim signal, this implies that, independently of whether the planet is magnetized or not, the mass-loss rate is small (\dot{M}_\star $\lesssim$ 0.3 \dot{M}_\sun) and that, concomitantly, the efficiency of the conversion of Poynting flux into radio emission must be low ($β\lesssim 10^{-3}$). Free-free absorption effects are negligible, given the high value of the coronal temperature. Finally, if the anisotropic beaming pointed away from us, this would imply that GJ~486 has very low values of its magnetic obliquity and inclination. |
| title | Searching for star-planet interactions in GJ 486 at radio wavelengths with the uGMRT |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2411.17689 |