How the breakout-limited mass in B-star centrifugal magnetospheres controls their circumstellar H-alpha emission
| Autor: | Stanley P. Owocki, J. O. Sundqvist, Matt Shultz, Steven R. Cranmer, Asif ud-Doula, Richard H. D. Townsend |
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| Jazyk: | angličtina |
| Rok vydání: | 2020 |
| Předmět: |
Astrophysics::High Energy Astrophysical Phenomena
Magnetosphere FOS: Physical sciences Field strength Trapping Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences 7. Clean energy symbols.namesake 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics Physics Breakout 010308 nuclear & particles physics Balmer series Astronomy and Astrophysics Stars Diffusion process Astrophysics - Solar and Stellar Astrophysics 13. Climate action Space and Planetary Science symbols Equivalent width |
| Popis: | Strongly magnetic B-type stars with moderately rapid rotation form `centrifugal magnetospheres' (CMs), from the magnetic trapping of stellar wind material in a region above the Kepler co-rotation radius. A longstanding question is whether the eventual loss of such trapped material occurs from gradual drift and/or diffusive leakage, or through sporadic `{\em centrifugal break out}' (CBO) events, wherein magnetic tension can no longer contain the built-up mass. We argue here that recent empirical results for Balmer-$\alpha$ emission from such B-star CMs strongly favor the CBO mechanism. Most notably, the fact that the onset of such emission depends mainly on the field strength at the Kepler radius, and is largely {\em independent} of the stellar luminosity, strongly disfavors any drift/diffusion process, for which the net mass balance would depend on the luminosity-dependent wind feeding rate. In contrast, we show that in a CBO model the {\em maximum confined mass} in the magnetosphere is independent of this wind feeding rate, and has a dependence on field strength and Kepler radius that naturally explains the empirical scalings for the onset of H$\alpha$ emission, its associated equivalent width, and even its line profile shapes. However, the general lack of observed Balmer emission in late-B and A-type stars could still be attributed to a residual level of diffusive or drift leakage that does not allow their much weaker winds to fill their CMs to the breakout level needed for such emission; alternatively this might result from a transition to a metal-ion wind that lacks the requisite Hydrogen. Comment: 13 pages, 11 figures, accepted for MNRAS |
| Databáze: | OpenAIRE |
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