6533b823fe1ef96bd127e2b0
RESEARCH PRODUCT
High Energy Emission and its Variability in Young Stellar Objects
Costanza ArgiroffiCostanza Argiroffisubject
starsYoung stellar objectAstrophysics::High Energy Astrophysical PhenomenaMagnetosphereFOS: Physical sciencesAstrophysicsAstrophysics::Cosmology and Extragalactic Astrophysics01 natural scienceslaw.inventionX-raySettore FIS/05 - Astronomia E Astrofisicaaccretionstarlaw0103 physical sciencesAstrophysics::Solar and Stellar Astrophysics010303 astronomy & astrophysicspremain sequenceSolar and Stellar Astrophysics (astro-ph.SR)Astrophysics::Galaxy AstrophysicsPhysicsHigh Energy Astrophysical Phenomena (astro-ph.HE)010308 nuclear & particles physicsactivityAstronomy and AstrophysicsPlasmaAccretion (astrophysics)StarsT Tauri starAstrophysics - Solar and Stellar AstrophysicsSpace and Planetary ScienceT Tauri starOutflowAstrophysics::Earth and Planetary AstrophysicsAstrophysics - High Energy Astrophysical PhenomenaFlaredescription
Young stars show a variety of highly energetic phenomena, from accretion and outflow processes to hot coronal plasmas confined in their outer atmosphere, all regulated by the intense stellar magnetic fields. Many aspects on each of these phenomena are debated, but, most notably, their complex mutual interaction remains obscure. In this work I report how these phenomena are simultaneously responsible for the high-energy emission from young stars, with a special focus on the expected and observed variability in the X-ray band. Investigating variations in the X-ray emission from young stars allows us to pose constraints on flare and coronal plasma properties, coronal heating, accretion stream properties, and accretion geometries. All these results are important building blocks for constructing a comprehensive picture of the complex magnetosphere of young stars.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2019-03-25 |