E-Print Archive

There are 4512 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Detection of stellar-like abundance anomalies in the slow solar wind View all abstracts by submitter

David Brooks   Submitted: 2022-04-20 21:06

The elemental composition of the Sun's hot atmosphere, the corona, shows a distinctive pattern that is different than the underlying surface, or photosphere (Pottasch 1963). Elements that are easy to ionize in the chromosphere are enhanced in abundance in the corona compared to their photospheric values. A similar pattern of behavior is often observed in the slow speed (< 500 km s-1) solar wind (Meyer 1985), and in solar-like stellar coronae (Drake et al. 1997), while a reversed effect is seen in M-dwarfs (Liefke et al. 2008). Studies of the inverse effect have been hampered in the past because only unresolved (point source) spectroscopic data were available for these stellar targets. Here we report the discovery of several inverse events observed in-situ in the slow solar wind using particle counting techniques. These very rare events all occur during periods of high solar activity that mimic conditions more widespread on M-dwarfs. The detections allow a new way of connecting the slow wind to its solar source, and are broadly consistent with theoretical models of abundance variations due to chromospheric fast mode waves with amplitudes of 8-10 km s-1; sufficient to accelerate the solar wind. The results imply that M-dwarf winds are dominated by plasma depleted in easily ionized elements, and lend credence to previous spectroscopic measurements.

Authors: David H. Brooks, Deborah Baker, Lidia van Driel-Gesztelyi, Harry P. Warren, Stephanie L. Yardley
Projects: ACE

Publication Status: To be published in ApJL
Last Modified: 2022-04-20 23:31
Go to main E-Print page  A Model of Homologous Confined and Ejective Eruptions Involving Kink Instability and Flux Cancellation  Magnetosheath jet occurrence rate in relation to CMEs and SIRs  Edit Entry  Download Preprint  Delete Entry 

Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
Grid-based imaging in X-rays and gamma-rays with high spatial resolution
It Takes a Village (Invited memoir)
Maximal growth rate of the ascending phase of a sunspot cycle for predicting its amplitude
Starspots Modelling and Flare Analysis on Selected MV Stars
Doubling of minute-long Quasi-Periodic Pulsations from super-flares on a low mass star
Geometric Assumptions in Hydrodynamic Modeling of Coronal and Flaring Loops
Sun-as-a-star Analysis of Hα Spectra of a Solar Flare Observed by SMART/SDDI: Time Evolution of Red Asymmetry and Line Broadening
Searching for quasi-periodic oscillations in astrophysical transients using Gaussian processes
Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption
Current-sheet Oscillations Caused by Kelvin-Helmholtz Instability at the Loop Top of Solar Flares
Annihilation of Magnetic Islands at the Top of Solar Flare Loops
Three-dimensional Magnetic and Thermodynamic Structures of Solar Microflares
Grow-up of a Filament Channel by Intermittent Small-scale Magnetic Reconnection
Small-scale solar jet formation and their associated waves and instabilities
Invited Review: Short-term Variability with the Observations from the Helioseismic and Magnetic Imager (HMI) Onboard the Solar Dynamics Observatory (SDO): Insights into Flare Magnetism
A first look at the submillimeter Sun with ALMA
Data-driven modeling of solar coronal magnetic field evolution and eruptions
Properties and Energetics of Magnetic Reconnection: I. Evolution of Flare Ribbons
A new look at the frequency-dependent damping of slow-mode waves in the solar corona
What determines active region coronal plasma composition?

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey

© 2000-2020 Solar Physics Group - Montana State University