TY - JOUR

T1 - Stellar Inclination Angles from Be-star Hα Emission Line Profiles

AU - Sigut, T. A.A.

AU - Mahjour, A. K.

AU - Tycner, C.

N1 - Publisher Copyright:
© 2020. The American Astronomical Society. All rights reserved.

PY - 2020/5/1

Y1 - 2020/5/1

N2 - We demonstrate that the angle between a star's rotation axis and the observer's line of sight, usually called the inclination angle, can be reliably determined for Be stars via Hα emission line profile fitting. We test our method on a sample of 11 Be stars with available long-baseline interferometric data from the Navy Precision Optical Interferometer. We fit the Hα emission line profile of each star to obtain a spectroscopic inclination angle i Hα. We then obtain an independent inclination angle estimate, iv2, by fitting the observed interferometric visibilities with model visibilities based on a purely geometric representation of the light distribution on the sky. The sample differences, {equation presented}, are normally distributed with a mean of zero and a standard deviation of 6.°7, and the linear correlation coefficient between i Hα and {equation presented} is r = 0.93. As Be stars comprise upwards of one-fifth of all main-sequence B-type stars, this Hα line profile fitting technique has the potential to provide an efficient method for detecting correlated stellar spin axes in young open clusters. Furthermore, if the orientation of the Be star's circumstellar disk on the plane of the sky can be constrained by polarization measurements, it is possible to determine the full 3D stellar rotation vector of each Be star.

AB - We demonstrate that the angle between a star's rotation axis and the observer's line of sight, usually called the inclination angle, can be reliably determined for Be stars via Hα emission line profile fitting. We test our method on a sample of 11 Be stars with available long-baseline interferometric data from the Navy Precision Optical Interferometer. We fit the Hα emission line profile of each star to obtain a spectroscopic inclination angle i Hα. We then obtain an independent inclination angle estimate, iv2, by fitting the observed interferometric visibilities with model visibilities based on a purely geometric representation of the light distribution on the sky. The sample differences, {equation presented}, are normally distributed with a mean of zero and a standard deviation of 6.°7, and the linear correlation coefficient between i Hα and {equation presented} is r = 0.93. As Be stars comprise upwards of one-fifth of all main-sequence B-type stars, this Hα line profile fitting technique has the potential to provide an efficient method for detecting correlated stellar spin axes in young open clusters. Furthermore, if the orientation of the Be star's circumstellar disk on the plane of the sky can be constrained by polarization measurements, it is possible to determine the full 3D stellar rotation vector of each Be star.

UR - http://www.scopus.com/inward/record.url?scp=85085293317&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/ab8386

DO - 10.3847/1538-4357/ab8386

M3 - Article

AN - SCOPUS:85085293317

SN - 0004-637X

VL - 894

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 18

ER -