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Constraining the stellar energetic particle flux in young solar-like stars

Published online by Cambridge University Press:  13 January 2020

Ch. Rab Open the ORCID record for Ch. Rab [Opens in a new window] ,
M. Padovani ,
M. Güdel ,
I. Kamp ,
W-F. Thi  and
P. Woitke
Ch. Rab
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands email: [email protected]
M. Padovani
Affiliation:
University of Vienna, Dept. of Astrophysics, Türkenschanzstr. 17, 1180 Wien, Austria
M. Güdel
Affiliation:
INAF-Ossevatorio Astrofisico di Arcetri, Largo E. Fermi, 5 - 50125 Firenze, Italy
I. Kamp
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands email: [email protected]
W-F. Thi
Affiliation:
MPE, Giessenbachstrasse 1, 85748 Garching, Germany
P. Woitke
Affiliation:
SUPA, School of Physics & Astronomy, University of St. Andrews, St. Andrews KY16 9SS, UK
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Abstract

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Anomalies in the abundance measurements of short lived radionuclides in meteorites indicate that the protosolar nebulae was irradiated by a large number of energetic particles (E≳ 10 MeV), often called solar cosmic rays. The particle flux of the contemporary Sun cannot explain these anomalies, but, similar to T Tauri stars, the young Sun was more active and probably produced enough high energy particles. However, the stellar particle (SP) flux of young stars is essentially unknown. We model the impact of high-energy ionization sources on the chemistry of the circumstellar environment (disks and envelopes). The model includes X-ray radiative transfer and makes use of particle transport models to calculate the individual molecular hydrogen ionization rates. We study the impact on the chemistry via the ionization tracers HCO+ and N2H+. We argue that spatially resolved observations of those molecules combined with detailed models allow for disentangling the contribution of the individual high-energy ionization sources and to put constraints on the SP flux in young stars.

Keywords

stars: pre–main-sequence(stars:) circumstellar matterstars: activityastrochemistryradiative transfermethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 310 - 311
Copyright
© International Astronomical Union 2020 

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