Bulletin of the American Physical Society
Mid-Atlantic Section 2022 Meeting
Volume 67, Number 20
Friday–Sunday, December 2–4, 2022; University Park, PA, Pennsylvania State University
Session C04: Astrophysics I
9:00 AM–10:35 AM,
Saturday, December 3, 2022
Pennsylvania State University
Room: Osmond 106
Chair: Tiffany Lewis, NASA Goddard Space Flight Center
Abstract: C04.00003 : Exploring the Initial B-Field Function of massive stars by simulating magnetic detectability in stars clusters*
9:47 AM–9:59 AM
Presenter:
Victor A Ramirez Delgado
(University of Delaware)
Authors:
Victor A Ramirez Delgado
(University of Delaware)
Véronique Petit
(Dept. Of Physics and Astronomy, Bartol Research Institute, University of Delaware)
Mary Oksala
(Dept. of Physics, California Lutheran University)
James MacDonald
(Dept. of Physics and Astronomy, University of Delaware)
Zsolt Keszthelyi
(Center for Computational Astrophysics, Division of Science, National Astronomical Observatory of Japan)
Ylva Götberg
(The Observatories of the Carnegie Institution for Science)
Shaquann S Seadrow
(University of Delaware)
Pinar Cerrahoglu
(University of Delaware)
The origin of stellar magnetic fields in intermediate- and high-mass stars remains an enigma in astronomy. Surveys find that about 10% of these stars in our galaxy exhibit globally organized magnetic fields without any apparent relationship with their stellar or rotational parameters. These magnetic fields are thought to be fossil fields, meaning they are purely dissipative, unlike dynamo-generated fields in low-mass stars. Taking into account the impact of fossil magnetic fields significantly changes their evolutionary tracks due to magnetic braking and mass-loss quenching. We present a study of synthetic star clusters generated with the population model MOSS and with MESA evolutionary models that account for the effects of magnetic braking and mass loss quenching. The values for the magnetic fields are assigned using various “Initial B-ield Functions” (IBF). Lastly, using current observational estimates from spectropolometric measurements, we infer how many stars in our simulated star clusters would have detectable B fields, assuming typical survey observing strategies. Our results show that higher temperatures and luminous stars are easier to detect than their counterparts at different cluster ages. We use these results to disentangle the role of observational biases from that of the true form of the IBF in explaining the properties of known magnetic massive stars.
*This work is supported by the National Science Foundation grant NSF AST-2108455.
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