The magnetic field of the B3V star 16 Pegasi

• Published in: Proceedings of the International Astronomical Union
• Main Authors: Henrichs, Hubertus F., Neiner, Coralie, Schnerr, R. S., Verdugo, Eva, Alecian, A., Catala, Claude, Cochard, François, Gutiérrez, Juan, Huat, Anne-Laure, Silvester, James, Thizy, Olivier
• Other Authors: Astronomical Institute, University of Amsterdam, Amsterdam, Netherlands, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique stellaire et galactique, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institute for Solar Physics, The Royal Swedish Academy of Sciences, European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Department of Physics, Royal Military College of Canada, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Shelyak Instruments, Strassmeier, Klaus G.; Kosovichev, Alexander G.; Beckman, John E.
• Format: Conference Object
• Language: English
• Published: HAL CCSD 2008
• Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]; narval
• Online Access: https://hal.science/hal-03734004; https://doi.org/10.1017/S1743921309030828

International audience The slowly pulsating B3V star 16 Pegasi was discovered by Hubrig et al. (2006) to be magnetic, based on low-resolution spectropolarimetric observations with FORS1 at the VLT. We have confirmed the presence of a magnetic field with new measurements with the spectropolarimeters Narval at TBL, France and Espadons at CFHT, Hawaii during 2007. The most likely period is about 1.44 d for the modulation of the field, but this could not be firmly established with the available data set. No variability has been found in the UV stellar wind lines. Although the star was reported once to show Halpha in emission, there exists at present no confirmation that the star is a Be star.