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The cool brown dwarf Gliese 229 B is a close binary

Fuente: arXiv

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Autores principales:	Xuan, Jerry W., Mérand, A., Thompson, W., Zhang, Y., Lacour, S., Blakely, D., Mawet, D., Oppenheimer, R., Kammerer, J., Batygin, K., Sanghi, A., Wang, J., Ruffio, J. -B., Liu, M. C., Knutson, H., Brandner, W., Burgasser, A., Rickman, E., Bowens-Rubin, R., Salama, M., Balmer, W., Blunt, S., Bourdarot, G., Caselli, P., Chauvin, G., Davies, R., Drescher, A., Eckart, A., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Förster, Garcia, P., Genzel, R., Gillessen, S., Grant, S., Hartl, M., Haußmann, F., Henning, T., Hinkley, S., Hönig, S. F., Horrobin, M., Houllé, M., Janson, M., Kervella, P., Kral, Q., Kreidberg, L., Bouquin, J. -B. Le, Lutz, D., Mang, F., Marleau, G. -D., Millour, F., More, N., Nowak, M., Ott, T., Otten, G., Paumard, T., Rabien, S., Rau, C., Ribeiro, D. C., Bordoni, M. Sadun, Sauter, J., Shangguan, J., Shimizu, T. T., Sykes, C., Soulain, A., Spezzano, S., Straubmeier, C., Stolker, T., Sturm, E., Subroweit, M., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Widmann, F., Wieprecht, E., Winterhalder, T. O., Woillez, J.
Formato:	Preprint
Publicado:	2024
Materias:	Solar and Stellar Astrophysics Earth and Planetary Astrophysics
Acceso en línea:	Acceder al recurso
Etiquetas:	Agregar Etiqueta Sin Etiquetas, Sea el primero en etiquetar este registro!

_version_	1866912073780297728
author	Xuan, Jerry W. Mérand, A. Thompson, W. Zhang, Y. Lacour, S. Blakely, D. Mawet, D. Oppenheimer, R. Kammerer, J. Batygin, K. Sanghi, A. Wang, J. Ruffio, J. -B. Liu, M. C. Knutson, H. Brandner, W. Burgasser, A. Rickman, E. Bowens-Rubin, R. Salama, M. Balmer, W. Blunt, S. Bourdarot, G. Caselli, P. Chauvin, G. Davies, R. Drescher, A. Eckart, A. Eisenhauer, F. Fabricius, M. Feuchtgruber, H. Finger, G. Schreiber, N. M. Förster Garcia, P. Genzel, R. Gillessen, S. Grant, S. Hartl, M. Haußmann, F. Henning, T. Hinkley, S. Hönig, S. F. Horrobin, M. Houllé, M. Janson, M. Kervella, P. Kral, Q. Kreidberg, L. Bouquin, J. -B. Le Lutz, D. Mang, F. Marleau, G. -D. Millour, F. More, N. Nowak, M. Ott, T. Otten, G. Paumard, T. Rabien, S. Rau, C. Ribeiro, D. C. Bordoni, M. Sadun Sauter, J. Shangguan, J. Shimizu, T. T. Sykes, C. Soulain, A. Spezzano, S. Straubmeier, C. Stolker, T. Sturm, E. Subroweit, M. Tacconi, L. J. van Dishoeck, E. F. Vigan, A. Widmann, F. Wieprecht, E. Winterhalder, T. O. Woillez, J.
author_facet	Xuan, Jerry W. Mérand, A. Thompson, W. Zhang, Y. Lacour, S. Blakely, D. Mawet, D. Oppenheimer, R. Kammerer, J. Batygin, K. Sanghi, A. Wang, J. Ruffio, J. -B. Liu, M. C. Knutson, H. Brandner, W. Burgasser, A. Rickman, E. Bowens-Rubin, R. Salama, M. Balmer, W. Blunt, S. Bourdarot, G. Caselli, P. Chauvin, G. Davies, R. Drescher, A. Eckart, A. Eisenhauer, F. Fabricius, M. Feuchtgruber, H. Finger, G. Schreiber, N. M. Förster Garcia, P. Genzel, R. Gillessen, S. Grant, S. Hartl, M. Haußmann, F. Henning, T. Hinkley, S. Hönig, S. F. Horrobin, M. Houllé, M. Janson, M. Kervella, P. Kral, Q. Kreidberg, L. Bouquin, J. -B. Le Lutz, D. Mang, F. Marleau, G. -D. Millour, F. More, N. Nowak, M. Ott, T. Otten, G. Paumard, T. Rabien, S. Rau, C. Ribeiro, D. C. Bordoni, M. Sadun Sauter, J. Shangguan, J. Shimizu, T. T. Sykes, C. Soulain, A. Spezzano, S. Straubmeier, C. Stolker, T. Sturm, E. Subroweit, M. Tacconi, L. J. van Dishoeck, E. F. Vigan, A. Widmann, F. Wieprecht, E. Winterhalder, T. O. Woillez, J.
contents	Owing to their similarities with giant exoplanets, brown dwarf companions of stars provide insights into the fundamental processes of planet formation and evolution. From their orbits, several brown dwarf companions are found to be more massive than theoretical predictions given their luminosities and the ages of their host stars (e.g. Brandt et al. 2021, Cheetham et al. 2018, Li et al. 2023). Either the theory is incomplete or these objects are not single entities. For example, they could be two brown dwarfs each with a lower mass and intrinsic luminosity (Brandt et al. 2021, Howe et al. 2024). The most problematic example is Gliese 229 B (Nakajima et al. 1995, Oppenheimer et al. 1995), which is at least 2-6 times less luminous than model predictions given its dynamical mass of $71.4\pm0.6$ Jupiter masses ($M_{\rm Jup}$) (Brandt et al. 2021). We observed Gliese 229 B with the GRAVITY interferometer and, separately, the CRIRES+ spectrograph at the Very Large Telescope. Both sets of observations independently resolve Gliese 229 B into two components, Gliese 229 Ba and Bb, settling the conflict between theory and observations. The two objects have a flux ratio of $0.47\pm0.03$ at a wavelength of 2 $μ$m and masses of $38.1\pm1.0$ and $34.4\pm1.5$ $M_{\rm Jup}$, respectively. They orbit each other every 12.1 days with a semimajor axis of 0.042 astronomical units (AU). The discovery of Gliese 229 BaBb, each only a few times more massive than the most massive planets, and separated by 16 times the Earth-moon distance, raises new questions about the formation and prevalence of tight binary brown dwarfs around stars.
format	Preprint
id	arxiv_https___arxiv_org_abs_2410_11953
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	The cool brown dwarf Gliese 229 B is a close binary Xuan, Jerry W. Mérand, A. Thompson, W. Zhang, Y. Lacour, S. Blakely, D. Mawet, D. Oppenheimer, R. Kammerer, J. Batygin, K. Sanghi, A. Wang, J. Ruffio, J. -B. Liu, M. C. Knutson, H. Brandner, W. Burgasser, A. Rickman, E. Bowens-Rubin, R. Salama, M. Balmer, W. Blunt, S. Bourdarot, G. Caselli, P. Chauvin, G. Davies, R. Drescher, A. Eckart, A. Eisenhauer, F. Fabricius, M. Feuchtgruber, H. Finger, G. Schreiber, N. M. Förster Garcia, P. Genzel, R. Gillessen, S. Grant, S. Hartl, M. Haußmann, F. Henning, T. Hinkley, S. Hönig, S. F. Horrobin, M. Houllé, M. Janson, M. Kervella, P. Kral, Q. Kreidberg, L. Bouquin, J. -B. Le Lutz, D. Mang, F. Marleau, G. -D. Millour, F. More, N. Nowak, M. Ott, T. Otten, G. Paumard, T. Rabien, S. Rau, C. Ribeiro, D. C. Bordoni, M. Sadun Sauter, J. Shangguan, J. Shimizu, T. T. Sykes, C. Soulain, A. Spezzano, S. Straubmeier, C. Stolker, T. Sturm, E. Subroweit, M. Tacconi, L. J. van Dishoeck, E. F. Vigan, A. Widmann, F. Wieprecht, E. Winterhalder, T. O. Woillez, J. Solar and Stellar Astrophysics Earth and Planetary Astrophysics Owing to their similarities with giant exoplanets, brown dwarf companions of stars provide insights into the fundamental processes of planet formation and evolution. From their orbits, several brown dwarf companions are found to be more massive than theoretical predictions given their luminosities and the ages of their host stars (e.g. Brandt et al. 2021, Cheetham et al. 2018, Li et al. 2023). Either the theory is incomplete or these objects are not single entities. For example, they could be two brown dwarfs each with a lower mass and intrinsic luminosity (Brandt et al. 2021, Howe et al. 2024). The most problematic example is Gliese 229 B (Nakajima et al. 1995, Oppenheimer et al. 1995), which is at least 2-6 times less luminous than model predictions given its dynamical mass of $71.4\pm0.6$ Jupiter masses ($M_{\rm Jup}$) (Brandt et al. 2021). We observed Gliese 229 B with the GRAVITY interferometer and, separately, the CRIRES+ spectrograph at the Very Large Telescope. Both sets of observations independently resolve Gliese 229 B into two components, Gliese 229 Ba and Bb, settling the conflict between theory and observations. The two objects have a flux ratio of $0.47\pm0.03$ at a wavelength of 2 $μ$m and masses of $38.1\pm1.0$ and $34.4\pm1.5$ $M_{\rm Jup}$, respectively. They orbit each other every 12.1 days with a semimajor axis of 0.042 astronomical units (AU). The discovery of Gliese 229 BaBb, each only a few times more massive than the most massive planets, and separated by 16 times the Earth-moon distance, raises new questions about the formation and prevalence of tight binary brown dwarfs around stars.
title	The cool brown dwarf Gliese 229 B is a close binary
topic	Solar and Stellar Astrophysics Earth and Planetary Astrophysics
url	https://arxiv.org/abs/2410.11953