Skip to main content Accessibility help
×
Home
Hostname: page-component-544b6db54f-bkjnw Total loading time: 0.144 Render date: 2021-10-22T23:33:56.686Z Has data issue: true Feature Flags: { "shouldUseShareProductTool": true, "shouldUseHypothesis": true, "isUnsiloEnabled": true, "metricsAbstractViews": false, "figures": true, "newCiteModal": false, "newCitedByModal": true, "newEcommerce": true, "newUsageEvents": true }

The Evolution of Surface Magnetic Fields in Young Solar-type Stars

Published online by Cambridge University Press:  27 January 2016

Colin P. Folsom
Affiliation:
Université Grenoble Alpes, IPAG, F-38000 Grenoble, France CNRS, IPAG, F-38000 Grenoble, France email: colin.folsom@obs.ujf-grenoble.fr
Pascal Petit
Affiliation:
IRAP, CNRS and Université de Toulouse, 14 avenue Édouard Belin, 31400, Toulouse, France
Jérôme Bouvier
Affiliation:
Université Grenoble Alpes, IPAG, F-38000 Grenoble, France CNRS, IPAG, F-38000 Grenoble, France email: colin.folsom@obs.ujf-grenoble.fr
Julien Morin
Affiliation:
LUPM, UMR 5299, CNRS and Université Montpellier II - Place E. Bataillon, 34090 Montpellier, France
Agnès Lèbre
Affiliation:
LUPM, UMR 5299, CNRS and Université Montpellier II - Place E. Bataillon, 34090 Montpellier, France
Jean-François Donati
Affiliation:
IRAP, CNRS and Université de Toulouse, 14 avenue Édouard Belin, 31400, Toulouse, France
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.

Surface rotation rates of young solar-type stars display drastic changes at the end of the pre-main sequence through the early main sequence. This may trigger corresponding changes in the magnetic dynamos operating in these stars, which ought to be observable in their surface magnetic fields. We present here the first results of an observational effort aimed at characterizing the evolution of stellar magnetic fields through this critical phase. We observed stars from open clusters and associations, which range from 20 to 600 Myr, and used Zeeman Doppler Imaging to characterize their complex magnetic fields. We find a clear trend towards weaker magnetic fields for older ages, as well as a tight correlation between magnetic field strength and Rossby number over this age range. Comparing to results for younger T Tauri stars, we observe a very significant change in magnetic strength and geometry, as the radiative core develops during the late pre-main sequence.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2016 

References

Bouvier, J. 2014 Protostars and Planets VI, 433Google Scholar
Donati, J.-F.et al. 2006, MNRAS, 370, 629CrossRefGoogle Scholar
Donati, J.-F.et al. 2011, MNRAS, 417, 1747CrossRefGoogle Scholar
Donati, J.-F.et al. 1997, MNRAS, 291, 658CrossRefGoogle Scholar
Gallet, F. & Bouvier, J. 2013 A&A, 556, A36Google Scholar
Gallet, F. & Bouvier, J. 2015 A&A, 577, A98Google Scholar
Gregory, S. G.et al. 2012 ApJ, 755, 97CrossRefGoogle Scholar
Matt, S. P., MacGregor, K. B., Pinsonneault, M. H., & Greene, T. P. 2012, ApJ, 754, L26CrossRefGoogle Scholar
Morin, J.et al. 2010, MNRAS, 407, 2269CrossRefGoogle Scholar
Petit, P.et al. 2008 MNRAS, 388, 80CrossRefGoogle Scholar
Vidotto, A. A.et al. 2014 MNRAS, 441, 2361CrossRefGoogle Scholar
You have Access

Send article to Kindle

To send this article to your Kindle, first ensure no-reply@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 sending to your Kindle. Find out more about sending to your Kindle.

Note you can select to send to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be sent 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.

The Evolution of Surface Magnetic Fields in Young Solar-type Stars
Available formats
×

Send article to Dropbox

To send 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 use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Dropbox.

The Evolution of Surface Magnetic Fields in Young Solar-type Stars
Available formats
×

Send article to Google Drive

To send 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 use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Google Drive.

The Evolution of Surface Magnetic Fields in Young Solar-type Stars
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? *