Tracing Accretion onto Herbig Ae/Be Stars Using the Br\gamma\ Line

• Published in: arXiv.org
• Main Authors: Grant, Sierra L, Espaillat, Catherine C, Brittain, Sean, Scott-Joseph, Caleb, Calvet, Nuria
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 21.12.2021
• Subjects: Accretion disks; Gratings (spectra); Infrared analysis; Infrared spectra; Luminosity; Massive stars; Near infrared radiation; Normalizing; Physics - Earth and Planetary Astrophysics; Physics - Solar and Stellar Astrophysics; Planet formation; Pre-main sequence stars; Protoplanetary disks; Stellar luminosity; Stellar mass; Stellar mass accretion; Tracing
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2112.10428

Accretion plays an important role in protoplanetary disk evolution, and it is thought that the accretion mechanism changes between low- and high-mass stars. Here, we characterize accretion in intermediate-mass, pre-main-sequence Herbig Ae/Be (HAeBe) stars to search for correlations between accretion and system properties. We present new high-resolution, near-infrared spectra from the Immersion GRating INfrared Spectrograph for 102 HAeBes and analyze the accretion-tracing Br\(\gamma\) line at 2.166 \(\mu\)m. We also include the samples of Fairlamb et al. and Donehew & Brittain, for a total of 155 targets. We find a positive correlation between the Br\(\gamma\) and stellar luminosity, with a change in the slope between the Herbig Aes and Herbig Bes. We use \(L_{Br\gamma}\) to determine the accretion luminosity and accretion rate. We find that the accretion luminosity and rate depend on stellar mass and age; however, the trend disappears when normalizing the accretion luminosity by the stellar luminosity. We classify the objects into flared (Group I) or flat (Group II) disks and find that there is no trend with accretion luminosity or rate, indicating that the disk dust structure is not impacting accretion. We test for Br\(\gamma\) variability in objects that are common to our sample and previous studies. We find that the Br\(\gamma\) line equivalent width is largely consistent between the literature observations and those that we present here, except in a few cases where we may be seeing changes in the accretion rate.