Accretion and magnetism on young eccentric binaries: DQ Tau and AK Sco

Author:

Pouilly Kim1ORCID,Hahlin Axel1,Kochukhov Oleg1ORCID,Morin Julien2ORCID,Kóspál Ágnes3456ORCID

Affiliation:

1. Department of Physics and Astronomy, Uppsala University , Box 516, SE-75120 Uppsala , Sweden

2. LUPM-UMR 5299, Université de Montpellier & CNRS , Place Eugene Bataillon, 34095 Montpellier, Cedex 05 , France

3. Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences , Konkoly-Thege Miklós út 15-17, H-1121 Budapest , Hungary

4. Max Planck Institute for Astronomy , Königstuhl 17, D-69117 Heidelberg , Germany

5. Institute of Physics, ELTE Eötvös Loránd University , Pázmány Péter sétány 1/A, H-1117 Budapest , Hungary

6. CSFK, MTA Centre of Excellence , Konkoly-Thege Miklós út 15-17, H-1121 Budapest , Hungary

Abstract

ABSTRACT The accretion and ejection of mass in pre-main-sequence (PMS) stars are key processes in stellar evolution as they shape the stellar angular momentum transport necessary for the stars’ stability. Magnetospheric accretion on to classical T Tauri stars and low-mass PMS stars has been widely studied in the single-star case. This process cannot be directly transferred to PMS binary systems, as tidal and gravitation effects, and/or accretion from a circumbinary disc (with variable separation of the components in the case of eccentric orbits) are in place. This work examines the accretion process of two PMS eccentric binaries, DQ Tau and AK Sco, using high-resolution spectropolarimetric time series. We investigate how magnetospheric accretion can be applied to these systems by studying the accretion-related emission lines and the magnetic field of each system. We discover that both systems are showing signs of magnetospheric accretion, despite their slightly different configurations, and the weak magnetic field of AK Sco. Furthermore, the magnetic topology of DQ Tau A shows a change relative to the previous orbital cycle studied: previously dominated by the poloidal component, it is now dominated by the toroidal component. We also report an increase of the component’s accretion and the absence of an accretion burst at the apastron, suggesting that the component’s magnetic variation might be the cause of the inter-cycle variations of the system’s accretion. We conclude on the presence of magnetospheric accretion for both systems, together with gravitational effects, especially for AK Sco, composed of more massive components.

Funder

ESO

Publisher

Oxford University Press (OUP)

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