Skip to main content Accessibility help
×
Home
Hostname: page-component-768ffcd9cc-b9rrs Total loading time: 0.479 Render date: 2022-12-07T07:28:20.706Z Has data issue: true Feature Flags: { "useRatesEcommerce": false } hasContentIssue true

Fast downflows in a chromospheric filament

Published online by Cambridge University Press:  24 September 2020

K. Sowmya
Affiliation:
Max-Planck-Institut für Sonnensystemforschung Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany email: krishnamurthy@mps.mpg.de
A. Lagg
Affiliation:
Max-Planck-Institut für Sonnensystemforschung Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany email: krishnamurthy@mps.mpg.de
S. K. Solanki
Affiliation:
Max-Planck-Institut für Sonnensystemforschung Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany email: krishnamurthy@mps.mpg.de School of Space Research, Kyung Hee University, YongIn, Gyeonggi 446–701, Korea
J. S. Castellanos Durán
Affiliation:
Max-Planck-Institut für Sonnensystemforschung Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany email: krishnamurthy@mps.mpg.de
Rights & Permissions[Opens in a new window]

Abstract

HTML view is not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

An active region filament in the upper chromosphere is studied using spectropolarimetric data in He i 10830 Å from the GREGOR telescope. A Milne-Eddingon based inversion of the Unno-Rachkovsky equations is used to retrieve the velocity and the magnetic field vector of the region. The plasma velocity reaches supersonic values closer to the feet of the filament barbs and coexist with a slow velocity component. Such supersonic velocities result from the acceleration of the plasma as it drains from the filament spine through the barbs. The line-of-sight magnetic fields have strengths below 200 G in the filament spine and in the filament barbs where fast downflows are located, their strengths range between 100 - 700 G.

Type
Contributed Papers
Copyright
© International Astronomical Union 2020

References

Collados, M., López, R., Páez, E., Hernández, E., Reyes, M., et al. 2012, AN, 333, 872CrossRefGoogle Scholar
Díaz Baso, C. J., Martínez González, M. J., & Asensio Ramos, A. 2019a, A&A, 625, A128CrossRefGoogle Scholar
Díaz Baso, C. J., Martínez González, M. J., & Asensio Ramos, A. 2019b, A&A, 625, A129CrossRefGoogle Scholar
Joshi, A. D., Srivastava, N., Mathew, S. K., & Martin, S. F. 2013, SoPh, 288, 191CrossRefGoogle Scholar
Kuckein, C., Centeno, R., Martínez Pillet, V., Casini, R., Manso Sainz, R., & Shimizu, T. 2009, A&A, 501, 1113CrossRefGoogle Scholar
Lagg, A., Woch, J., Krupp, N., & Solanki, S. K. 2004, A&A, 414, 1109CrossRefGoogle Scholar
Lagg, A., Ishikawa, R., Merenda, L., Wiegelmann, T., Tsuneta, S., & Solanki, S. K. 2009, ASPC, 415, 327Google Scholar
Sasso, C., Lagg, A., & Solanki, S. K. 2011, A&A, 526, A42CrossRefGoogle Scholar
Sasso, C., Lagg, A., & Solanki, S. K. 2014, A&A, 561, A98CrossRefGoogle Scholar
Schmidt, W., von der Lühe, O., Volkmer, R., Denker, C., Solanki, S. K., et al. 2012, Astronomische Nachrichten, 333, 796CrossRefGoogle Scholar
You have Access

Save article to Kindle

To save this article to your Kindle, first ensure coreplatform@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about saving to your Kindle.

Note you can select to save to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be saved to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

Find out more about the Kindle Personal Document Service.

Fast downflows in a chromospheric filament
Available formats
×

Save article to Dropbox

To save this article to your Dropbox account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you used this feature, you will be asked to authorise Cambridge Core to connect with your Dropbox account. Find out more about saving content to Dropbox.

Fast downflows in a chromospheric filament
Available formats
×

Save article to Google Drive

To save this article to your Google Drive account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you used this feature, you will be asked to authorise Cambridge Core to connect with your Google Drive account. Find out more about saving content to Google Drive.

Fast downflows in a chromospheric filament
Available formats
×
×

Reply to: Submit a response

Please enter your response.

Your details

Please enter a valid email address.

Conflicting interests

Do you have any conflicting interests? *