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Wolf 327b: A new member of the pack of ultra-short-period super-Earths around M dwarfs

Fuente: arXiv

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Autori principali:	Murgas, F., Pallé, E., Orell-Miquel, J., Carleo, I., Peña-Moñino, L., Pérez-Torres, M., Watkins, C. N., Jeffers, S. V., Azzaro, M., Barkaoui, K., Belinski, A. A., Caballero, J. A., Charbonneau, D., Cheryasov, D. V., Ciardi, D. R., Collins, K. A., Cortés-Contreras, M., de Leon, J., Duque-Arribas, C., Enoc, G., Esparza-Borges, E., Fukui, A., Geraldía-González, S., Gilbert, E. A., Hatzes, A. P., Hayashi, Y., Henning, Th., Herrero, E., Jenkins, J. M., Lillo-Box, J., Lodieu, N., Lund, M. B., Luque, R., Montes, D., Nagel, E., Narita, N., Parviainen, H., Polanski, A. S., Reffert, S., Schlecker, M., Schöfer, P., Schwarz, R. P., Schweitzer, A., Seager, S., Stassun, K. G., Tabernero, H. M., Terada, Y., Twicken, J. D., Vanaverbeke, S., Winn, J. N., Zambelli, R., Amado, P. J., Quirrenbach, A., Reiners, A., Ribas, I.
Natura:	Preprint
Pubblicazione:	2024
Soggetti:	Earth and Planetary Astrophysics Solar and Stellar Astrophysics
Accesso online:	Acceder al recurso
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_version_	1866913203820167168
author	Murgas, F. Pallé, E. Orell-Miquel, J. Carleo, I. Peña-Moñino, L. Pérez-Torres, M. Watkins, C. N. Jeffers, S. V. Azzaro, M. Barkaoui, K. Belinski, A. A. Caballero, J. A. Charbonneau, D. Cheryasov, D. V. Ciardi, D. R. Collins, K. A. Cortés-Contreras, M. de Leon, J. Duque-Arribas, C. Enoc, G. Esparza-Borges, E. Fukui, A. Geraldía-González, S. Gilbert, E. A. Hatzes, A. P. Hayashi, Y. Henning, Th. Herrero, E. Jenkins, J. M. Lillo-Box, J. Lodieu, N. Lund, M. B. Luque, R. Montes, D. Nagel, E. Narita, N. Parviainen, H. Polanski, A. S. Reffert, S. Schlecker, M. Schöfer, P. Schwarz, R. P. Schweitzer, A. Seager, S. Stassun, K. G. Tabernero, H. M. Terada, Y. Twicken, J. D. Vanaverbeke, S. Winn, J. N. Zambelli, R. Amado, P. J. Quirrenbach, A. Reiners, A. Ribas, I.
author_facet	Murgas, F. Pallé, E. Orell-Miquel, J. Carleo, I. Peña-Moñino, L. Pérez-Torres, M. Watkins, C. N. Jeffers, S. V. Azzaro, M. Barkaoui, K. Belinski, A. A. Caballero, J. A. Charbonneau, D. Cheryasov, D. V. Ciardi, D. R. Collins, K. A. Cortés-Contreras, M. de Leon, J. Duque-Arribas, C. Enoc, G. Esparza-Borges, E. Fukui, A. Geraldía-González, S. Gilbert, E. A. Hatzes, A. P. Hayashi, Y. Henning, Th. Herrero, E. Jenkins, J. M. Lillo-Box, J. Lodieu, N. Lund, M. B. Luque, R. Montes, D. Nagel, E. Narita, N. Parviainen, H. Polanski, A. S. Reffert, S. Schlecker, M. Schöfer, P. Schwarz, R. P. Schweitzer, A. Seager, S. Stassun, K. G. Tabernero, H. M. Terada, Y. Twicken, J. D. Vanaverbeke, S. Winn, J. N. Zambelli, R. Amado, P. J. Quirrenbach, A. Reiners, A. Ribas, I.
contents	Planets with orbital periods shorter than 1 day are rare and have formation histories that are not completely understood. Small ($R_\mathrm{p} < 2\; R_\oplus$) ultra-short-period (USP) planets are highly irradiated, probably have rocky compositions with high bulk densities, and are often found in multi-planet systems. Additionally, USP planets found around small stars are excellent candidates for characterization using present-day instrumentation. Of the current full sample of approximately 5500 confirmed exoplanets, only 130 are USP planets and around 40 have mass and radius measurements. Wolf 327 (TOI-5747) is an M dwarf ($R_\star = 0.406 \pm 0.015 \; R_\odot$, $M_\star = 0.405 \pm 0.019 \; M_\odot$, $T_{\mathrm{eff}}=3542 \pm 70$ K, and $V = 13$ mag) located at a distance $d = 28.5$ pc. NASA's planet hunter satellite, TESS, detected transits in this star with a period of 0.573 d (13.7 h) and with a transit depth of 818 ppm. Ground-based follow-up photometry, high resolution imaging, and radial velocity (RV) measurements taken with the CARMENES spectrograph confirm the presence of this new USP planet. Wolf 327b is a super-Earth with a radius of $R_\mathrm{p} = 1.24 \pm 0.06 \; R_\oplus$ and a mass of $M_\mathrm{p} = 2.53 \pm 0.46 \; M_\oplus$, yielding a bulk density of $7.24 \pm 1.66 $\,g cm$^{-3}$ and thus suggesting a rocky composition. Owing to its close proximity to its host star ($a = 0.01$ au), Wolf 327b has an equilibrium temperature of $996 \pm 22$ K. This planet has a mass and radius similar to K2-229b, a planet with an inferred Mercury-like internal composition. Planet interior models suggest that Wolf 327b has a large iron core, a small rocky mantle, and a negligible (if any) H/He atmosphere.
format	Preprint
id	arxiv_https___arxiv_org_abs_2401_12150
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	Wolf 327b: A new member of the pack of ultra-short-period super-Earths around M dwarfs Murgas, F. Pallé, E. Orell-Miquel, J. Carleo, I. Peña-Moñino, L. Pérez-Torres, M. Watkins, C. N. Jeffers, S. V. Azzaro, M. Barkaoui, K. Belinski, A. A. Caballero, J. A. Charbonneau, D. Cheryasov, D. V. Ciardi, D. R. Collins, K. A. Cortés-Contreras, M. de Leon, J. Duque-Arribas, C. Enoc, G. Esparza-Borges, E. Fukui, A. Geraldía-González, S. Gilbert, E. A. Hatzes, A. P. Hayashi, Y. Henning, Th. Herrero, E. Jenkins, J. M. Lillo-Box, J. Lodieu, N. Lund, M. B. Luque, R. Montes, D. Nagel, E. Narita, N. Parviainen, H. Polanski, A. S. Reffert, S. Schlecker, M. Schöfer, P. Schwarz, R. P. Schweitzer, A. Seager, S. Stassun, K. G. Tabernero, H. M. Terada, Y. Twicken, J. D. Vanaverbeke, S. Winn, J. N. Zambelli, R. Amado, P. J. Quirrenbach, A. Reiners, A. Ribas, I. Earth and Planetary Astrophysics Solar and Stellar Astrophysics Planets with orbital periods shorter than 1 day are rare and have formation histories that are not completely understood. Small ($R_\mathrm{p} < 2\; R_\oplus$) ultra-short-period (USP) planets are highly irradiated, probably have rocky compositions with high bulk densities, and are often found in multi-planet systems. Additionally, USP planets found around small stars are excellent candidates for characterization using present-day instrumentation. Of the current full sample of approximately 5500 confirmed exoplanets, only 130 are USP planets and around 40 have mass and radius measurements. Wolf 327 (TOI-5747) is an M dwarf ($R_\star = 0.406 \pm 0.015 \; R_\odot$, $M_\star = 0.405 \pm 0.019 \; M_\odot$, $T_{\mathrm{eff}}=3542 \pm 70$ K, and $V = 13$ mag) located at a distance $d = 28.5$ pc. NASA's planet hunter satellite, TESS, detected transits in this star with a period of 0.573 d (13.7 h) and with a transit depth of 818 ppm. Ground-based follow-up photometry, high resolution imaging, and radial velocity (RV) measurements taken with the CARMENES spectrograph confirm the presence of this new USP planet. Wolf 327b is a super-Earth with a radius of $R_\mathrm{p} = 1.24 \pm 0.06 \; R_\oplus$ and a mass of $M_\mathrm{p} = 2.53 \pm 0.46 \; M_\oplus$, yielding a bulk density of $7.24 \pm 1.66 $\,g cm$^{-3}$ and thus suggesting a rocky composition. Owing to its close proximity to its host star ($a = 0.01$ au), Wolf 327b has an equilibrium temperature of $996 \pm 22$ K. This planet has a mass and radius similar to K2-229b, a planet with an inferred Mercury-like internal composition. Planet interior models suggest that Wolf 327b has a large iron core, a small rocky mantle, and a negligible (if any) H/He atmosphere.
title	Wolf 327b: A new member of the pack of ultra-short-period super-Earths around M dwarfs
topic	Earth and Planetary Astrophysics Solar and Stellar Astrophysics
url	https://arxiv.org/abs/2401.12150