Solar CME Plasma Diagnostics Expressed as Potential Stellar CME Signatures
arXiv:2205.12985 · doi:10.3847/1538-3881/ac80c4
Abstract
Solar coronal mass ejections (CMEs) have a strong association with solar flares that is not fully understood. This characteristic of our Sun's magnetic activity may also occur on other stars, but the lack of successfully detected stellar CMEs makes it difficult to perform statistical studies that might show a similar association between CMEs and flares. Because of the potentially strong association, the search for stellar CMEs often starts with a successful search for superflares on magnetically active stars. Regardless of the flare's presence, we emphasize the utility of searching for CME-specific spectroscopic signatures when attempting to find and confirm stellar CME candidates. We use solar CMEs as examples of why a multitude of ultraviolet emission lines, when detected simultaneously, can substantially improve the credibility of spectroscopically discovered stellar CME candidates. We make predictions on how bright CME-related emission lines can be if they derived from distant stars. We recommend the use of three emission lines in particular (C IV 1550 Angstroms, O VI 1032 Angstroms, and C III 977 Angstroms) due to their potentially bright signal and convenient diagnostic capabilities that can be used to confirm if an observational signature truly derives from a stellar CME.
References in corpus (13)
- CHIANTI - an atomic database for emission lines - Paper XV: Version 9, improvements for the X-ray satellite lines
- Probable detection of an eruptive filament from a superflare on a solar-type star
- The Stellar CME-flare relation: What do historic observations reveal?
- A stellar flare-coronal mass ejection event revealed by X-ray plasma motions
- The quest for stellar coronal mass ejections in late-type stars: I. Investigating Balmer-line asymmetries of single stars in Virtual Observatory data
- Scaling laws of solar and stellar flares
- Automatic Detection and Tracking of CMEs II: Multiscale Filtering of Coronagraph Data
- Plasma Heating During a Coronal Mass Ejection Observed by SOHO
- Exploring Plasma Heating in the Current Sheet Region in a Three-Dimensional Coronal Mass Ejection Simulation
- Coronal Mass Ejections and Dimmings: A Comparative Study using MHD Simulations and SDO Observations
- The Effect of Solar Wind Expansion and Non-Equilibrium Ionization on the Broadening of Coronal Emission Lines
- Opacity in the upper atmospheres of active stars II. AD Leonis
- Constraining the CME Core Heating and Energy Budget with SOHO/UVCS