Spectroscopic signatures of magnetospheric accretion in Herbig Ae/Be stars. I. The case of HD101412

TL;DR

This study investigates magnetospheric accretion in the Herbig Ae star HD101412 using near-infrared spectroscopy, revealing rotational modulation of accretion signatures and suggesting accretion occurs near magnetic poles.

Contribution

First to detect rotational modulation of accretion signatures in a Herbig Ae star, linking spectroscopic variability to magnetic field geometry.

Findings

Detected a 20.53-day rotational period from spectroscopic lines.

Found accretion occurs near magnetic poles intersecting the line-of-sight.

Confirmed magnetospheric accretion signatures in Herbig Ae star HD101412.

Abstract

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. 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 HD101412. We used near-infrared spectroscopic observations of the magnetic Herbig Ae star HD101412 to test the magnetospheric character of its accretion disk/star interaction. We reduced and analyzed 30 spectra of HD101412, acquired with the CRIRES and X-shooter spectrographs installed at the VLT (ESO, Chile). The spectroscopic analysis was based on the He I lambda 10,830 and Pa gamma lines, formed in the accretion region. We found that the temporal behavior of these diagnostic lines in the near-infrared spectra of HD101412 can be explained by rotational modulation of line profiles generated by accreting gas with a period P = 20.53+-1.68 d. The discovery of this period, about half of the magnetic rotation period P_m = 42.076 d 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.