Origin of Radio-quiet Coronal Mass Ejections in Flare Stars

Thumbnail Image

Files

1902.00810.pdf (512.79 KB)

Links to Files

https://iopscience.iop.org/article/10.3847/1538-4357/ab041b

Permanent Link

https://arxiv.org/abs/1902.00810
 http://hdl.handle.net/11603/24256

Collections

UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)

Author/Creator

Author/Creator ORCID

https://orcid.org/0000-0002-8090-3570

Date

2019-02-27

Type of Work

journal articles
preprints
Text

Department

Program

Citation of Original Publication

Mullan, D. J. and Rishi R. Paudel. The Astrophysical Journal 873 (Feb. 27, 2019), no. 1. https://doi.org/10.3847/1538-4357/ab041b.

Rights

© 2019. The American Astronomical Society. All rights reserved

Subjects

Abstract

Type II radio bursts are observed in the Sun in association with many coronal mass ejections (CMEs). In view of this association, there has been an expectation that, by scaling from solar flares to the flares that are observed on M dwarfs, radio emission analogous to solar type II bursts should be detectable in association with M dwarf flares. However, several surveys have revealed that this expectation does not seem to be fulfilled. Here we hypothesize that the presence of larger global field strengths in low-mass stars, suggested by recent magnetoconvective modeling, gives rise to such large Alfvén speeds in the corona that it becomes difficult to satisfy the conditions for the generation of type II radio bursts. As a result, CMEs propagating in the corona/wind of flare stars are expected to be "radio-quiet" as regards type II bursts. In view of this, we suggest that, in the context of type II bursts, scaling from solar to stellar flares is of limited effectiveness.