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

F. Murgas; E. Pallé; J. Orell-Miquel; I. Carleo; L. Peña-Moñino; M. Pérez-Torres; C. N. Watkins; S. V. Jeffers; M. Azzaro; K. Barkaoui; A. A. Belinski; J. A. Caballero; D. Charbonneau; D. V. Cheryasov; D. R. Ciardi; K. A. Collins; M. Cortés-Contreras; J. de Leon; C. Duque-Arribas; G. Enoc; E. Esparza-Borges; A. Fukui; S. Geraldía-González; E. A. Gilbert; A. P. Hatzes; Y. Hayashi; Th Henning; E. Herrero; J. M. Jenkins; J. Lillo-Box; N. Lodieu; M. B. Lund; R. Luque; D. Montes; E. Nagel; N. Narita; H. Parviainen; A. S. Polanski; S. Reffert; M. Schlecker; P. Schöfer; R. P. Schwarz; A. Schweitzer; S. Seager; K. G. Stassun; H. M. Tabernero; Y. Terada; J. D. Twicken; S. Vanaverbeke; J. N. Winn; R. Zambelli; P. J. Amado; A. Quirrenbach; A. Reiners; I. Ribas

doi:10.1051/0004-6361/202348813

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

F. Murgas, E. Pallé, J. Orell-Miquel, I. Carleo, L. Peña-Moñino, M. Pérez-Torres, C. N. Watkins, S. V. Jeffers, M. Azzaro, K. Barkaoui, A. A. Belinski, J. A. Caballero, D. Charbonneau, D. V. Cheryasov, D. R. Ciardi, K. A. Collins, M. Cortés-Contreras, J. de Leon, C. Duque-Arribas, G. EnocE. Esparza-Borges, A. Fukui, S. Geraldía-González, E. A. Gilbert, A. P. Hatzes, Y. Hayashi, Th Henning, E. Herrero, J. M. Jenkins, J. Lillo-Box, N. Lodieu, M. B. Lund, R. Luque, D. Montes, E. Nagel, N. Narita, H. Parviainen, A. S. Polanski, S. Reffert, M. Schlecker, P. Schöfer, R. P. Schwarz, A. Schweitzer, S. Seager, K. G. Stassun, H. M. Tabernero, Y. Terada, J. D. Twicken, S. Vanaverbeke, J. N. Winn, R. Zambelli, P. J. Amado, A. Quirrenbach, A. Reiners, I. Ribas

Astrophysical Sciences

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Abstract

Planets with orbital periods shorter than 1 day are rare and have formation histories that are not completely understood. Small (R_p < 2 R_⊕) 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_★ = 0.406 ± 0.015 R_☉, M_★ = 0.405 ± 0.019 M_☉, T_eff = 3542 ± 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 day (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_p = 1.24 ± 0.06 R_⊕ and a mass of M_p = 2.53 ± 0.46 M_⊕, yielding a bulk density of 7.24 ± 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 ± 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.

Original language	English (US)
Article number	A83
Journal	Astronomy and Astrophysics
Volume	684
DOIs	https://doi.org/10.1051/0004-6361/202348813
State	Published - Apr 1 2024

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

planets and satellites: detection
planets and satellites: terrestrial planets
stars: individual: Wolf 327
stars: late-type
techniques: photometric
techniques: radial velocities

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10.1051/0004-6361/202348813

Cite this

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., ... Ribas, I. (2024). Wolf 327b: A new member of the pack of ultra-short-period super-Earths around M dwarfs. Astronomy and Astrophysics, 684, Article A83. https://doi.org/10.1051/0004-6361/202348813

@article{0a4567d9e7894d5bb2043305c2d9f8f0,

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

abstract = "Planets with orbital periods shorter than 1 day are rare and have formation histories that are not completely understood. Small (Rp < 2 R⊕) 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★ = 0.406 ± 0.015 R☉, M★ = 0.405 ± 0.019 M☉, Teff = 3542 ± 70 K, and V = 13 mag) located at a distance d = 28.5 pc. NASA{\textquoteright}s planet hunter satellite, TESS, detected transits in this star with a period of 0.573 day (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 Rp = 1.24 ± 0.06 R⊕ and a mass of Mp = 2.53 ± 0.46 M⊕, yielding a bulk density of 7.24 ± 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 ± 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.",

keywords = "planets and satellites: detection, planets and satellites: terrestrial planets, stars: individual: Wolf 327, stars: late-type, techniques: photometric, techniques: radial velocities",

author = "F. Murgas and E. Pall{\'e} and J. Orell-Miquel and I. Carleo and L. Pe{\~n}a-Mo{\~n}ino and M. P{\'e}rez-Torres and Watkins, {C. N.} and Jeffers, {S. V.} and M. Azzaro and K. Barkaoui and Belinski, {A. A.} and Caballero, {J. A.} and D. Charbonneau and Cheryasov, {D. V.} and Ciardi, {D. R.} and Collins, {K. A.} and M. Cort{\'e}s-Contreras and {de Leon}, J. and C. Duque-Arribas and G. Enoc and E. Esparza-Borges and A. Fukui and S. Gerald{\'i}a-Gonz{\'a}lez and Gilbert, {E. A.} and Hatzes, {A. P.} and Y. Hayashi and Th Henning and E. Herrero and Jenkins, {J. M.} and J. Lillo-Box and N. Lodieu and Lund, {M. B.} and R. Luque and D. Montes and E. Nagel and N. Narita and H. Parviainen and Polanski, {A. S.} and S. Reffert and M. Schlecker and P. Sch{\"o}fer and Schwarz, {R. P.} and A. Schweitzer and S. Seager and Stassun, {K. G.} and Tabernero, {H. M.} and Y. Terada and Twicken, {J. D.} and S. Vanaverbeke and Winn, {J. N.} and R. Zambelli and Amado, {P. J.} and A. Quirrenbach and A. Reiners and I. Ribas",

note = "Publisher Copyright: {\textcopyright} The Authors 2024.",

year = "2024",

month = apr,

day = "1",

doi = "10.1051/0004-6361/202348813",

language = "English (US)",

volume = "684",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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Murgas, F, Pallé, E, Orell-Miquel, J, Carleo, I, Peña-Moñino, L, Pérez-Torres, M, Watkins, CN, Jeffers, SV, Azzaro, M, Barkaoui, K, Belinski, AA, Caballero, JA, Charbonneau, D, Cheryasov, DV, Ciardi, DR, Collins, KA, Cortés-Contreras, M, de Leon, J, Duque-Arribas, C, Enoc, G, Esparza-Borges, E, Fukui, A, Geraldía-González, S, Gilbert, EA, Hatzes, AP, Hayashi, Y, Henning, T, Herrero, E, Jenkins, JM, Lillo-Box, J, Lodieu, N, Lund, MB, Luque, R, Montes, D, Nagel, E, Narita, N, Parviainen, H, Polanski, AS, Reffert, S, Schlecker, M, Schöfer, P, Schwarz, RP, Schweitzer, A, Seager, S, Stassun, KG, Tabernero, HM, Terada, Y, Twicken, JD, Vanaverbeke, S, Winn, JN, Zambelli, R, Amado, PJ, Quirrenbach, A, Reiners, A & Ribas, I 2024, 'Wolf 327b: A new member of the pack of ultra-short-period super-Earths around M dwarfs', Astronomy and Astrophysics, vol. 684, A83. https://doi.org/10.1051/0004-6361/202348813

TY - JOUR

T1 - Wolf 327b

T2 - A new member of the pack of ultra-short-period super-Earths around M dwarfs

AU - Murgas, F.

AU - Pallé, E.

AU - Orell-Miquel, J.

AU - Carleo, I.

AU - Peña-Moñino, L.

AU - Pérez-Torres, M.

AU - Watkins, C. N.

AU - Jeffers, S. V.

AU - Azzaro, M.

AU - Barkaoui, K.

AU - Belinski, A. A.

AU - Caballero, J. A.

AU - Charbonneau, D.

AU - Cheryasov, D. V.

AU - Ciardi, D. R.

AU - Collins, K. A.

AU - Cortés-Contreras, M.

AU - de Leon, J.

AU - Duque-Arribas, C.

AU - Enoc, G.

AU - Esparza-Borges, E.

AU - Fukui, A.

AU - Geraldía-González, S.

AU - Gilbert, E. A.

AU - Hatzes, A. P.

AU - Hayashi, Y.

AU - Henning, Th

AU - Herrero, E.

AU - Jenkins, J. M.

AU - Lillo-Box, J.

AU - Lodieu, N.

AU - Lund, M. B.

AU - Luque, R.

AU - Montes, D.

AU - Nagel, E.

AU - Narita, N.

AU - Parviainen, H.

AU - Polanski, A. S.

AU - Reffert, S.

AU - Schlecker, M.

AU - Schöfer, P.

AU - Schwarz, R. P.

AU - Schweitzer, A.

AU - Seager, S.

AU - Stassun, K. G.

AU - Tabernero, H. M.

AU - Terada, Y.

AU - Twicken, J. D.

AU - Vanaverbeke, S.

AU - Winn, J. N.

AU - Zambelli, R.

AU - Amado, P. J.

AU - Quirrenbach, A.

AU - Reiners, A.

AU - Ribas, I.

PY - 2024/4/1

Y1 - 2024/4/1

N2 - Planets with orbital periods shorter than 1 day are rare and have formation histories that are not completely understood. Small (Rp < 2 R⊕) 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★ = 0.406 ± 0.015 R☉, M★ = 0.405 ± 0.019 M☉, Teff = 3542 ± 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 day (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 Rp = 1.24 ± 0.06 R⊕ and a mass of Mp = 2.53 ± 0.46 M⊕, yielding a bulk density of 7.24 ± 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 ± 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.

AB - Planets with orbital periods shorter than 1 day are rare and have formation histories that are not completely understood. Small (Rp < 2 R⊕) 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★ = 0.406 ± 0.015 R☉, M★ = 0.405 ± 0.019 M☉, Teff = 3542 ± 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 day (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 Rp = 1.24 ± 0.06 R⊕ and a mass of Mp = 2.53 ± 0.46 M⊕, yielding a bulk density of 7.24 ± 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 ± 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.

KW - planets and satellites: detection

KW - planets and satellites: terrestrial planets

KW - stars: individual: Wolf 327

KW - stars: late-type

KW - techniques: photometric

KW - techniques: radial velocities

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U2 - 10.1051/0004-6361/202348813

DO - 10.1051/0004-6361/202348813

M3 - Article

AN - SCOPUS:85190307158

SN - 0004-6361

VL - 684

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A83

ER -

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

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