This is a Be star showing emission features in its Balmer lines due to a circumstellar disk of decreated gas. It is classified as a suspected Gamma Cassiopeiae type variable star with a visual magnitude varying from +4.30 down to +4.39.
The star is classified as a Be star displaying emission in its Balmer lines, which are attributed to a circumstellar disk of disintegrated gas. It is suspected to be a Gamma Cassiopeiae type variable with visual magnitude variations ranging from +4.30 to +4.39.