The APOGEE view of Be stars

Bibcode
2014AAS...22340307E
Zasowski, G.; Wilson, J. C.; Nidever, D. L.; Schneider, D. P.; Skrutskie, M. F.; Holtzman, J. A.; Li, Z.; Meszaros, S.; Garner, A.; Hearty, F.; Davenport, J. R.; Ebelke, G.; Feuillet, D.; Borish, H.; Whelan, D. G.; Bizyaev, D.; Wisniewski, J. P.; Majewski, S. R.; Shetrone, M. D.; Chojnowski, S.; Eikenberry, Stephen S.
Bibliographical reference

American Astronomical Society, AAS Meeting #223, #403.07

Advertised on:
1
2014
Number of authors
21
IAC number of authors
1
Citations
0
Refereed citations
0
Description
I will present an overview of the 100+ previously unidentified Be stars discovered during the APOGEE survey. I will particularly focus on the new highly-magnetized Rigidly Rotating Magnetosphere (RRM) stars of the Sigma Orionis E type we have found. Both of the discovered stars show the spectroscopic signatures of the rigidly rotating magnetospheres common to this class of highly-magnetized (B ˜10 kiloGauss) stars. One (ABES-050) is an early main-sequence B star with unusually strong He absorption (similar to Sig Ori E), while the other (ABES-075) appears to be “He-normal” with a B3 IV subtype - the first known magnetized RRM star that is He-normal and possibly off the main sequence. We combine the APOGEE discovery spectra with other optical and near-infrared spectra of these two stars, as well as of Sig Ori E itself, to show how near-infrared spectroscopy can be a powerful tool for discovering more of these rare objects. We discuss the potential for further discovery of Sig Ori E type stars, as well as the implications of our discoveries for the population of these objects and insights into their origin and evolution.
Type
Non-refereed

It may interest you

  • Non-refereed
    Einasto Gravitational Potentials have Difficulty to Hold Spherically Symmetric Stellar Systems with Cores
    It was known that an ideal spherically symmetric stellar system with isotropic velocities and an inner core cannot reside in a Navarro, Frenk, and White (NFW) gravitational potential. The incompatibility can be pinned down to the radial gradient of the NFW potential in the very center of the system, which differs from zero. The gradient is
    Sánchez Almeida, Jorge

    Advertised on:

    6
    2024
    Bibcode
    2024RNAAS...8..167S
    Citations
    0
  • Non-refereed
    The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201
    Measuring the obliquities of stars hosting giant planets may shed light on the dynamical history of planetary systems. Significant efforts have been made to measure the obliquities of FGK stars with hot Jupiters, mainly based on observations of the Rossiter–McLaughlin effect. In contrast, M dwarfs with hot Jupiters have hardly been explored because
    Gan, Tianjun et al.

    Advertised on:

    7
    2024
    Bibcode
    2024ApJ...969L..24G
  • Non-refereed
    A Systematic Search for and Characterization of White Dwarf Binaries Across the H-R Diagram
    White dwarfs (WDs) are the endpoint of evolution for 97% of stars. Most of these stars are in multiple systems, and a significant fraction of those are compact enough to exchange mass, altering the structures and subsequent evolution of both stars. The physical mechanisms that facilitate these mass exchanges include common envelope evolution, Roche
    Anguiano, Borja et al.

    Advertised on:

    6
    2024
    Bibcode
    2024AAS...24410807A
    Citations
    0