English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
  Coronal Mass Ejections and Type II Radio Emission Variability during a Magnetic Cycle on the Solar-type Star ϵ Eridani

Fionnagáin, D. Ó., Kavanagh, R. D., Vidotto, A. A., Jeffers, S. V., Petit, P., Marsden, S., et al. (2022). Coronal Mass Ejections and Type II Radio Emission Variability during a Magnetic Cycle on the Solar-type Star ϵ Eridani. The Astrophysical Journal, 924(2): 115. doi:10.3847/1538-4357/ac35de.

Item is

Basic

show hide
Genre: Journal Article
Other : Coronal Mass Ejections and Type II Radio Emission Variability during a Magnetic Cycle on the Solar-type Star epsilon Eridani

Files

show Files

Locators

show

Creators

show
hide
 Creators:
Fionnagáin, Dúalta Ó, Author
Kavanagh, Robert D., Author
Vidotto, Aline A., Author
Jeffers, Sandra V.1, Author           
Petit, Pascal, Author
Marsden, Stephen, Author
Morin, Julien, Author
Golden, Aaron, Author
BCool Collaboration, Author              
Affiliations:
1Department Solar and Stellar Interiors, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832287              

Content

show
hide
Free keywords: Magnetohydrodynamical simulations; Radio bursts; Stellar winds; Stellar coronal mass ejections
 Abstract: We simulate possible stellar coronal mass ejection (CME) scenarios over the magnetic cycle of epsilon Eridani (18 Eridani; HD 22049). We use three separate epochs from 2008, 2011, and 2013, and estimate the radio emission frequencies associated with these events. These stellar eruptions have proven to be elusive, although a promising approach to detect and characterize these phenomena are low-frequency radio observations of potential type II bursts as CME-induced shocks propagate through the stellar corona. Stellar type II radio bursts are expected to emit below 450 MHz, similarly to their solar counterparts. We show that the length of time these events remain above the ionospheric cutoff is not necessarily dependent on the stellar magnetic cycle, but more on the eruption location relative to the stellar magnetic field. We find that these type II bursts would remain within the frequency range of LOFAR for a maximum of 20–30 minutes post-eruption for the polar CMEs (50 minutes for second harmonics). We find evidence of slower equatorial CMEs, which result in slightly longer observable windows for the 2008 and 2013 simulations. Stellar magnetic geometry and strength have a significant effect on the detectability of these events. We place the CMEs in the context of the stellar mass-loss rate (27–48× solar mass-loss rate), showing that they can amount to 3%–50% of the stellar wind mass-loss rate for epsilon Eridani. Continuous monitoring of likely stellar CME candidates with low-frequency radio telescopes will be required to detect these transient events.

Details

show
hide
Language(s): eng - English
 Dates: 2022
 Publication Status: Published online
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.3847/1538-4357/ac35de
 Degree: -

Event

show

Legal Case

show

Project information

show

Source 1

show
hide
Title: The Astrophysical Journal
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: Bristol; Vienna : IOP Publishing; IAEA
Pages: - Volume / Issue: 924 (2) Sequence Number: 115 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3