TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS

Autor: Bonfanti, A., Gandolfi, D., Egger, J. A., Fossati, L., Cabrera, J., Krenn, A., Alibert, Y., Benz, W., Billot, N., Florén, H. -G., Lendl, M., Adibekyan, V., Salmon, S., Santos, N. C., Sousa, S. G., Wilson, T. G., Barragán, O., Cameron, A. Collier, Delrez, L., Esposito, M., Goffo, E., Osborne, H., Osborn, H. P., Serrano, L. M., Van Eylen, V., Alarcon, J., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Bedell, M., Bonfils, X., Borsato, L., Brandeker, A., Broeg, C., Charnoz, S., Van Damme, C. Corral, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Demangeon, O. D. S., Demory, B. -O., Ehrenreich, D., Erikson, A., Fortier, A., Fridlund, M., Gillon, M., Güdel, M., Hoyer, S., Isaak, K. G., Kerschbaum, F., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lorenzo-Oliveira, D., Lovis, C., Magrin, D., Marafatto, L., Maxted, P. F. L., Meléndez, J., Mordasini, C., Nascimbeni, V., 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., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, Gy. M., Thomas, N., Udry, S., Ulmer, B., Van Grootel, V., Venturini, J., Walton, N. A.

Publikováno v: A&A 671, L8 (2023)

TOI-1055 is a Sun-like star known to host a transiting Neptune-sized planet on a 17.5-day orbit (TOI-1055 b). Radial velocity (RV) analyses carried out by two independent groups using nearly the same set of HARPS spectra have provided measurements of

Externí odkaz: http://arxiv.org/abs/2302.10664

Coherent radio emission from a quiescent red dwarf indicative of star-planet interaction

Autor: Vedantham, H. K., Callingham, J. R., Shimwell, T. W., Tasse, C., Pope, B. J. S., Bedell, M., Snellen, I., Best, P., Hardcastle, M. J., Haverkorn, M., Mechev, A., O'Sullivan, S. P., Röttgering, H. J. A., White, G. J.

Low frequency ($\nu\lesssim 150\,$MHz) stellar radio emission is expected to originate in the outer corona at heights comparable to and larger than the stellar radius. Such emission from the Sun has been used to study coronal structure, mass ejection

Externí odkaz: http://arxiv.org/abs/2002.08727

The Solar Twin Planet Search III. The [Y/Mg] clock: estimating stellar ages of solar-type stars

Autor: Maia, M. Tucci, Ramírez, I., Meléndez, J., Bedell, M., Bean, J. L., Asplund, M.

Publikováno v: A&A 590, A32 (2016)

Solar twins are stars with similar stellar (surface) parameters to the Sun that can have a wide range of ages. This provide an opportunity to analyze the variation of their chemical abundances with age. Nissen (2015) recently suggested that the abund

Externí odkaz: http://arxiv.org/abs/1604.05733

Stellar Chemical Abundances: In Pursuit of the Highest Achievable Precision

Autor: Bedell, M., Melendez, J., Bean, J., Ramirez, I., Leite, P., Asplund, M.

The achievable level of precision on photospheric abundances of stars is a major limiting factor on investigations of exoplanet host star characteristics, the chemical histories of star clusters, and the evolution of the Milky Way and other galaxies.

Externí odkaz: http://arxiv.org/abs/1409.1230

18 Sco: a solar twin rich in refractory and neutron-capture elements. Implications for chemical tagging

Autor: Melendez, J., Ramirez, I., Karakas, A. I., Yong, D., Monroe, T. R., Bedell, M., Bergemann, M., Asplund, M., Maia, M. Tucci, Bean, J., Nascimento, J. -D. do, Bazot, M., Alves-Brito, A., Freitas, F. C., Castro, M.

We study with unprecedented detail the chemical composition and stellar parameters of the solar twin 18 Sco in a strictly differential sense relative to the Sun. Our study is mainly based on high resolution (R ~ 110 000) high S/N (800-1000) VLT UVES

Externí odkaz: http://arxiv.org/abs/1406.5244