Buchumschlag

A possible misaligned orbit for the young planet AU Mic c

Fuente: arXiv

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Bibliographische Detailangaben
Hauptverfasser:	Yu, H., Garai, Z., Cretignier, M., Szabó, Gy. M., Aigrain, S., Gandolfi, D., Bryant, E. M., Correia, A. C. M., Klein, B., Brandeker, A., Owen, J. E., Günther, M. N., Winn, J. N., Heitzmann, A., Cegla, H. M., Wilson, T. G., Gill, S., Kriskovics, L., Barragán, O., Boldog, A., Nielsen, L. D., Billot, N., Lafarga, M., Meech, A., Alibert, Y., Alonso, R., Bárczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Bayliss, D., Benz, W., Bergomi, M., Borsato, L., Broeg, C., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Demangeon, O. D. S., Demory, B. O., Derekas, A., Doyle, L., Edwards, B., Egger, J. A., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gazeas, K., Gillon, M., Güdel, M., Helling, Ch., Isaak, K. G., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Magrin, D., Maxted, P. F. L., McCormac, J., Merín, B., Mordasini, C., Nascimbeni, V., O'Brien, S. M., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Southworth, R., Stalport, M., Steinberger, M., Sulis, S., Udry, S., Ulmer, B., Ulmer-Moll, S., Van Grootel, V., Venturini, J., Villaver, E., Walton, N. A., Wheatley, P. J.
Format:	Preprint
Veröffentlicht:	2024
Schlagworte:	Earth and Planetary Astrophysics Instrumentation and Methods for Astrophysics Solar and Stellar Astrophysics
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author	Yu, H. Garai, Z. Cretignier, M. Szabó, Gy. M. Aigrain, S. Gandolfi, D. Bryant, E. M. Correia, A. C. M. Klein, B. Brandeker, A. Owen, J. E. Günther, M. N. Winn, J. N. Heitzmann, A. Cegla, H. M. Wilson, T. G. Gill, S. Kriskovics, L. Barragán, O. Boldog, A. Nielsen, L. D. Billot, N. Lafarga, M. Meech, A. Alibert, Y. Alonso, R. Bárczy, T. Barrado, D. Barros, S. C. C. Baumjohann, W. Bayliss, D. Benz, W. Bergomi, M. Borsato, L. Broeg, C. Cameron, A. Collier Csizmadia, Sz. Cubillos, P. E. Davies, M. B. Deleuil, M. Deline, A. Demangeon, O. D. S. Demory, B. O. Derekas, A. Doyle, L. Edwards, B. Egger, J. A. Ehrenreich, D. Erikson, A. Fortier, A. Fossati, L. Fridlund, M. Gazeas, K. Gillon, M. Güdel, M. Helling, Ch. Isaak, K. G. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Magrin, D. Maxted, P. F. L. McCormac, J. Merín, B. Mordasini, C. Nascimbeni, V. O'Brien, S. M. Olofsson, G. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Piazza, D. Piotto, G. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Rauer, H. Ribas, I. Santos, N. C. Scandariato, G. Ségransan, D. Simon, A. E. Smith, A. M. S. Sousa, S. G. Southworth, R. Stalport, M. Steinberger, M. Sulis, S. Udry, S. Ulmer, B. Ulmer-Moll, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A. Wheatley, P. J.
author_facet	Yu, H. Garai, Z. Cretignier, M. Szabó, Gy. M. Aigrain, S. Gandolfi, D. Bryant, E. M. Correia, A. C. M. Klein, B. Brandeker, A. Owen, J. E. Günther, M. N. Winn, J. N. Heitzmann, A. Cegla, H. M. Wilson, T. G. Gill, S. Kriskovics, L. Barragán, O. Boldog, A. Nielsen, L. D. Billot, N. Lafarga, M. Meech, A. Alibert, Y. Alonso, R. Bárczy, T. Barrado, D. Barros, S. C. C. Baumjohann, W. Bayliss, D. Benz, W. Bergomi, M. Borsato, L. Broeg, C. Cameron, A. Collier Csizmadia, Sz. Cubillos, P. E. Davies, M. B. Deleuil, M. Deline, A. Demangeon, O. D. S. Demory, B. O. Derekas, A. Doyle, L. Edwards, B. Egger, J. A. Ehrenreich, D. Erikson, A. Fortier, A. Fossati, L. Fridlund, M. Gazeas, K. Gillon, M. Güdel, M. Helling, Ch. Isaak, K. G. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Magrin, D. Maxted, P. F. L. McCormac, J. Merín, B. Mordasini, C. Nascimbeni, V. O'Brien, S. M. Olofsson, G. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Piazza, D. Piotto, G. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Rauer, H. Ribas, I. Santos, N. C. Scandariato, G. Ségransan, D. Simon, A. E. Smith, A. M. S. Sousa, S. G. Southworth, R. Stalport, M. Steinberger, M. Sulis, S. Udry, S. Ulmer, B. Ulmer-Moll, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A. Wheatley, P. J.
contents	The AU Microscopii planetary system is only 24 Myr old, and its geometry may provide clues about the early dynamical history of planetary systems. Here, we present the first measurement of the Rossiter-McLaughlin effect for the warm sub-Neptune AU Mic c, using two transits observed simultaneously with the European Southern Observatory's (ESO's) Very Large Telescope (VLT)/Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO), CHaracterising ExOPlanet Satellite (CHEOPS), and Next-Generation Transit Survey (NGTS). After correcting for flares and for the magnetic activity of the host star, and accounting for transit-timing variations, we find the sky-projected spin-orbit angle of planet c to be in the range $λ_c=67.8_{-49.0}^{+31.7}$\,degrees (1-$σ$). We examine the possibility that planet c is misaligned with respect to the orbit of the inner planet b ($λ_b=-2.96_{-10.30}^{+10.44}$\,degrees), and the equatorial plane of the host star, and discuss scenarios that could explain both this and the planet's high density, including secular interactions with other bodies in the system or a giant impact. We note that a significantly misaligned orbit for planet c is in some degree of tension with the dynamical stability of the system, and with the fact that we see both planets in transit, though these arguments alone do not preclude such an orbit. Further observations would be highly desirable to constrain the spin-orbit angle of planet c more precisely.
format	Preprint
id	arxiv_https___arxiv_org_abs_2411_16958
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	A possible misaligned orbit for the young planet AU Mic c Yu, H. Garai, Z. Cretignier, M. Szabó, Gy. M. Aigrain, S. Gandolfi, D. Bryant, E. M. Correia, A. C. M. Klein, B. Brandeker, A. Owen, J. E. Günther, M. N. Winn, J. N. Heitzmann, A. Cegla, H. M. Wilson, T. G. Gill, S. Kriskovics, L. Barragán, O. Boldog, A. Nielsen, L. D. Billot, N. Lafarga, M. Meech, A. Alibert, Y. Alonso, R. Bárczy, T. Barrado, D. Barros, S. C. C. Baumjohann, W. Bayliss, D. Benz, W. Bergomi, M. Borsato, L. Broeg, C. Cameron, A. Collier Csizmadia, Sz. Cubillos, P. E. Davies, M. B. Deleuil, M. Deline, A. Demangeon, O. D. S. Demory, B. O. Derekas, A. Doyle, L. Edwards, B. Egger, J. A. Ehrenreich, D. Erikson, A. Fortier, A. Fossati, L. Fridlund, M. Gazeas, K. Gillon, M. Güdel, M. Helling, Ch. Isaak, K. G. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Magrin, D. Maxted, P. F. L. McCormac, J. Merín, B. Mordasini, C. Nascimbeni, V. O'Brien, S. M. Olofsson, G. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Piazza, D. Piotto, G. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Rauer, H. Ribas, I. Santos, N. C. Scandariato, G. Ségransan, D. Simon, A. E. Smith, A. M. S. Sousa, S. G. Southworth, R. Stalport, M. Steinberger, M. Sulis, S. Udry, S. Ulmer, B. Ulmer-Moll, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A. Wheatley, P. J. Earth and Planetary Astrophysics Instrumentation and Methods for Astrophysics Solar and Stellar Astrophysics The AU Microscopii planetary system is only 24 Myr old, and its geometry may provide clues about the early dynamical history of planetary systems. Here, we present the first measurement of the Rossiter-McLaughlin effect for the warm sub-Neptune AU Mic c, using two transits observed simultaneously with the European Southern Observatory's (ESO's) Very Large Telescope (VLT)/Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO), CHaracterising ExOPlanet Satellite (CHEOPS), and Next-Generation Transit Survey (NGTS). After correcting for flares and for the magnetic activity of the host star, and accounting for transit-timing variations, we find the sky-projected spin-orbit angle of planet c to be in the range $λ_c=67.8_{-49.0}^{+31.7}$\,degrees (1-$σ$). We examine the possibility that planet c is misaligned with respect to the orbit of the inner planet b ($λ_b=-2.96_{-10.30}^{+10.44}$\,degrees), and the equatorial plane of the host star, and discuss scenarios that could explain both this and the planet's high density, including secular interactions with other bodies in the system or a giant impact. We note that a significantly misaligned orbit for planet c is in some degree of tension with the dynamical stability of the system, and with the fact that we see both planets in transit, though these arguments alone do not preclude such an orbit. Further observations would be highly desirable to constrain the spin-orbit angle of planet c more precisely.
title	A possible misaligned orbit for the young planet AU Mic c
topic	Earth and Planetary Astrophysics Instrumentation and Methods for Astrophysics Solar and Stellar Astrophysics
url	https://arxiv.org/abs/2411.16958