On the Frequency of Field Galactic Be Stars

2005/09/07 by J. Zorec, Juan Zorec, Zorec, Juan +3 · 1 citation
Engineering · Physics and Astronomy · #Astronomical Observations and Instrumentation #Astrophysics (astro-ph) #FOS: Physical sciences #History and Developments in Astronomy #Stellar, planetary, and galactic studies #astro-ph

paper · pdf · doi:10.48550/arxiv.astro-ph/0509170

Societe Francaise d'Astronomie et d'Astrophysique, France (2005)

arxiv created 2005/09/07 · openalex publication_date 2005/09/07 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28

Abstract

Since Be stars belong to the high velocity tail of a single B star velocity distribution, the appearance of the Be phenomenon must be independent of the stellar mass. In the present paper we show that the shape of the distribution of the number fraction N(Be)/N(Be+B) against the spectral type can be explained in terms of the Balmer line emission efficiency as a function of the effective temperature.

Cited by

• Classical Be stars

Related

• Spectroscopic atlas of Hαand Hβin a sample of northern Be stars
• Evolution of Galactic Field be Stars
• Study of the Balmer decrements for Galactic classical Be stars using the Himalayan Chandra Telescope of India
• BRITEning up the Be Phenomenon
• Be Stars Seen by Space Photometry