6533b82bfe1ef96bd128d90d
RESEARCH PRODUCT
Star-disk interaction in classical T Tauri stars revealed using wavelet analysis
Giuseppina MicelaJavier López-santiagoFabio RealeFabio RealeS. SciortinoEttore FlaccomioI. Crespo-chacónsubject
010504 meteorology & atmospheric sciencesStars: flareAstrophysics::High Energy Astrophysical PhenomenaFOS: Physical sciencesX-rays: starsContext (language use)Astrophysics01 natural sciencesSettore FIS/05 - Astronomia E Astrofisica0103 physical sciencesOrion NebulaDifferential rotationAstrophysics::Solar and Stellar Astrophysics010303 astronomy & astrophysicsSolar and Stellar Astrophysics (astro-ph.SR)Astrophysics::Galaxy Astrophysics0105 earth and related environmental sciencesPhysicsCoronal seismologyHigh Energy Astrophysical Phenomena (astro-ph.HE)Stellar atmosphereAstronomy and AstrophysicsCoronaT Tauri starStarsAstrophysics - Solar and Stellar AstrophysicsSpace and Planetary SciencePhysics::Space PhysicsAstrophysics::Earth and Planetary AstrophysicsAstrophysics - High Energy Astrophysical Phenomenadescription
The extension of the corona of classical T Tauri stars (CTTS) is under discussion. The standard model of magnetic configuration of CTTS predicts that coronal magnetic flux tubes connect the stellar atmosphere to the inner region of the disk. However, differential rotation may disrupt these long loops. The results from Hydrodynamic modeling of X-ray flares observed in CTTS confirming the star-disk connection hypothesis are still controversial. Some authors suggest the presence of the accretion disk prevent the stellar corona to extent beyond the co-rotation radius, while others simply are not confident with the methods used to derive loop lengths. We use independent procedures to determine the length of flaring loops in stars of the Orion Nebula Cluster previously analyzed using Hydrodynamic models. Our aim is to disentangle between the two scenarios proposed. We present a different approach to determine the length of flaring loops based on the oscillatory nature of the loops after strong flares. We use wavelet tools to reveal oscillations during several flares. The subsequent analysis of such oscillations is settle on the Physics of coronal seismology. Our results likely confirm the large extension of the corona of CTTS and the hypothesis of star-disk magnetic interaction in at least three CTTS of the Orion Nebula Cluster. Analyzing oscillations in flaring events is a powerful tool to determine the physical characteristics of magnetic loops in coronae in stars other than the Sun. The results presented in this work confirm the star-disk magnetic connection in CTTS.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2016-03-19 |