Matches in SemOpenAlex for { <https://semopenalex.org/work/W3088174927> ?p ?o ?g. }
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- W3088174927 abstract "Rapidly rotating early-type stars with strong magnetic fields frequently show H$alpha$ emission originating in Centrifugal Magnetospheres (CMs), circumstellar structures in which centrifugal support due to magnetically enforced corotation of the magnetically confined plasma enables it to accumulate to high densities. It is not currently known whether the CM plasma escapes via Centrifugal Breakout (CB), or by an unidentified leakage mechanism. We have conducted the first comprehensive examination of the H$alpha$ emission properties of all stars currently known to display CM-pattern emission. We find that the onset of emission is dependent primarily on the area of the CM, which can be predicted simply by the value $B_{rm K}$ of the magnetic field at the Kepler corotation radius $R_{rm K}$. Emission strength is strongly sensitive to both CM area and $B_{rm K}$. Emission onset and strength are {em not} dependent on effective temperature, luminosity, or mass-loss rate. These results all favour a CB scenario, however the lack of intrinsic variability in any CM diagnostics indicates that CB must be an essentially continuous process, i.e. it effectively acts as a leakage mechanism. We also show that the emission profile shapes are approximately scale-invariant, i.e. they are broadly similar across a wide range of emission strengths and stellar parameters. While the radius of maximum emission correlates closely as expected to $R_{rm K}$, it is always larger, contradicting models that predict that emission should peak at $R_{rm K}$." @default.
- W3088174927 created "2020-10-01" @default.
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- W3088174927 date "2020-10-23" @default.
- W3088174927 modified "2023-10-09" @default.
- W3088174927 title "The magnetic early B-type stars – IV. Breakout or leakage? H α emission as a diagnostic of plasma transport in centrifugal magnetospheres" @default.
- W3088174927 cites W130970736 @default.
- W3088174927 cites W1550615391 @default.
- W3088174927 cites W1690662531 @default.
- W3088174927 cites W1759537663 @default.
- W3088174927 cites W1899577895 @default.
- W3088174927 cites W1912983829 @default.
- W3088174927 cites W1932775044 @default.
- W3088174927 cites W1942829712 @default.
- W3088174927 cites W1967126567 @default.
- W3088174927 cites W1969096257 @default.
- W3088174927 cites W1971089222 @default.
- W3088174927 cites W1989430366 @default.
- W3088174927 cites W2006322889 @default.
- W3088174927 cites W2010330193 @default.
- W3088174927 cites W2014776579 @default.
- W3088174927 cites W2019225886 @default.
- W3088174927 cites W2022805524 @default.
- W3088174927 cites W2029381501 @default.
- W3088174927 cites W2037174982 @default.
- W3088174927 cites W2050404632 @default.
- W3088174927 cites W2062508708 @default.
- W3088174927 cites W2064035408 @default.
- W3088174927 cites W2067283665 @default.
- W3088174927 cites W2068843564 @default.
- W3088174927 cites W2072318577 @default.
- W3088174927 cites W2072650474 @default.
- W3088174927 cites W2073773626 @default.
- W3088174927 cites W2074634711 @default.
- W3088174927 cites W2079180914 @default.
- W3088174927 cites W2085720473 @default.
- W3088174927 cites W2087822966 @default.
- W3088174927 cites W2088623414 @default.
- W3088174927 cites W2097434693 @default.
- W3088174927 cites W2098038777 @default.
- W3088174927 cites W2106841830 @default.
- W3088174927 cites W2111778853 @default.
- W3088174927 cites W2116480638 @default.
- W3088174927 cites W2118272902 @default.
- W3088174927 cites W2125312481 @default.
- W3088174927 cites W2130154861 @default.
- W3088174927 cites W2135319545 @default.
- W3088174927 cites W2136704211 @default.
- W3088174927 cites W2150586101 @default.
- W3088174927 cites W2156226566 @default.
- W3088174927 cites W2158780475 @default.
- W3088174927 cites W2165523878 @default.
- W3088174927 cites W2166099130 @default.
- W3088174927 cites W2170076045 @default.
- W3088174927 cites W2170971640 @default.
- W3088174927 cites W2257738445 @default.
- W3088174927 cites W2258695975 @default.
- W3088174927 cites W2266014535 @default.
- W3088174927 cites W2345822663 @default.
- W3088174927 cites W2407226508 @default.
- W3088174927 cites W2530872504 @default.
- W3088174927 cites W2554732597 @default.
- W3088174927 cites W2560067519 @default.
- W3088174927 cites W2575070387 @default.
- W3088174927 cites W2595923693 @default.
- W3088174927 cites W2730998929 @default.
- W3088174927 cites W2742639978 @default.
- W3088174927 cites W2757806101 @default.
- W3088174927 cites W2770257652 @default.
- W3088174927 cites W2770328861 @default.
- W3088174927 cites W2773345113 @default.
- W3088174927 cites W2782904071 @default.
- W3088174927 cites W2898814202 @default.
- W3088174927 cites W2898883686 @default.
- W3088174927 cites W2913789340 @default.
- W3088174927 cites W2917550843 @default.
- W3088174927 cites W2971759341 @default.
- W3088174927 cites W3000864472 @default.
- W3088174927 cites W3098059682 @default.
- W3088174927 cites W3098992598 @default.
- W3088174927 cites W3099571084 @default.