Volume 592, August 2016
|Number of page(s)||8|
|Published online||22 July 2016|
Spectroscopic signatures of magnetospheric accretion in Herbig Ae/Be stars
I. The case of HD 101412 ⋆
1 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
2 Central Astronomical Observatory at Pulkovo, Pulkovskoye chaussee 65, 196140 Saint Petersburg, Russia
3 I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
4 Saint Petersburg State University, Universitetskiy pr. 28, 198504 Saint Petersburg, Russia
5 Observatório Nacional/MCTI, Rua General José Cristino 77, CEP 20921-400, Rio de Janeiro, RJ, Brazil
6 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
7 Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya 48, 119017 Moscow, Russia
8 Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE), 5400 San Juan, Argentina
9 INAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
Received: 21 February 2016
Accepted: 24 May 2016
Context. Models of magnetically-driven accretion and outflows reproduce many observational properties of T Tauri stars. This concept is not well established for the more massive Herbig Ae/Be stars.
Aims. We intend to examine the magnetospheric accretion in Herbig Ae/Be stars and search for rotational modulation using spectroscopic signatures, in this first paper concentrating on the well-studied Herbig Ae star HD 101412.
Methods. We used near-infrared spectroscopic observations of the magnetic Herbig Ae star HD 101412 to test the magnetospheric character of its accretion disk/star interaction. We reduced and analyzed 30 spectra of HD 101412, acquired with the CRIRES and X-shooter spectrographs installed at the VLT (ESO, Chile). The spectroscopic analysis was based on the He iλ10 830 and Paγ lines, formed in the accretion region.
Results. We found that the temporal behavior of these diagnostic lines in the near-infrared spectra of HD 101412 can be explained by rotational modulation of line profiles generated by accreting gas with a period . The discovery of this period, about half of the magnetic rotation period previously determined from measurements of the mean longitudinal magnetic field, indicates that the accreted matter falls onto the star in regions close to the magnetic poles intersecting the line-of-sight two times during the rotation cycle. We intend to apply this method to a larger sample of Herbig Ae/Be stars.
Key words: stars: pre-main sequence / accretion, accretion disks / stars: magnetic field / stars: individual: HD101412
© ESO, 2016
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