Abstract
Several space missions and instruments for UV spectropolarimetry are in preparation, such as the proposed NASA MIDEX Polstar project, the proposed ESA M mission Arago, and the Pollux instrument on the future LUVOIR-like NASA flagship mission. In the frame of Polstar, we have studied the capabilities these observatories would offer to gain information on the magnetic and plasma properties of the magnetospheres of hot stars, helping us test the fundamental hypothesis that magnetospheres should act to rapidly drain angular momentum, thereby spinning the star down, whilst simultaneously reducing the net mass-loss rate. Both effects are expected to lead to dramatic differences in the evolution of magnetic vs. non-magnetic stars.
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Data sharing not applicable to this article as no datasets were generated or analysed during the current study.
Notes
Unless the star is critically rotating, in which case \(R_{\mathrm{K}}\) becomes identical to the equatorial radius; while theoretically possible, no such object has been found, and in any case such a phase would be extremely short-lived due to strong magnetic braking.
This diagnostic is unavailable for O-type stars, since the large radio photospheres produced by their dense winds swallow any gyrosynchrotron radiation produced by their magnetospheres (e.g. Chandra et al. 2015).
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Funding
AuD acknowledges support by NASA through Chandra Award number TM1-22001B and GO2-23003X issued by the Chandra X-ray Observatory 27 Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060.
M.E.S. acknowledges financial support from the Annie Jump Cannon Fellowship, supported by the University of Delaware and endowed by the Mount Cuba Astronomical Observatory.
A.D.-U. is supported by NASA under award number 80GSFC21M0002.
C.E. gratefully acknowledges support for this work provided by NASA through grant number HST-AR-15794.001-A from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. C.E. also gratefully acknowledges support from the National Science Foundation under Grant No. AST-2009412.
M.C.M.C. acknowledges internal research support from Lockheed Martin Advanced Technology Center.
This material is based upon work supported by the National Center for Atmospheric Research, which is a major facility sponsored by the National Science Foundation under Cooperative Agreement No. 1852977.
Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the European Space Agency (ESA) and the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Programme (contracts linked to XMM-Newton and Gaia).
N.S. acknowledges support provided by NAWA through grant number PPN/SZN/2020/1/00016/U/DRAFT/00001/U/00001.
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ud-Doula, A., Cheung, M.C.M., David-Uraz, A. et al. Ultraviolet spectropolarimetric diagnostics of hot star magnetospheres. Astrophys Space Sci 367, 117 (2022). https://doi.org/10.1007/s10509-022-04097-8
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DOI: https://doi.org/10.1007/s10509-022-04097-8