50 Persei
A white main-sequence star with multiple variable classifications and a debris disk.
50 Persei is a white main-sequence star of spectral type F7V located approximately 21.00 parsecs away in the constellation Perseus. With an apparent magnitude of 5.52, it is bright enough to be seen with the naked eye. The star is notable for its variable classifications and for being part of a probable multiple-star system.
- Apparent magnitude
- 5.52
- Distance
- 21.00 pc
- Spectral type
- F7V
- Variable type
- Candidate Gamma Doradus variable; subsequently classified as RS Canum Venaticorum and BY Draconis variable
- Period
- 3.05 days
- Infrared excess
- 70 μm
- Angular separation of hip 19255 componen
- 3.87″
Lore & Background
In 1998, 50 Persei was named a candidate Gamma Doradus variable with a period of 3.05 days, indicating luminosity variations due to non-radial pulsations in its photosphere. Later, an automated program classified it as both an RS Canum Venaticorum and a BY Draconis variable. The star is probably a binary system with an unseen companion. It is physically associated with the likely binary system HIP 19255, with the two pairs orbiting each other over a time scale of around a million years. The components of HIP 19255 have an angular separation of 3.87″ and orbit each other every 590 years. 50 Persei may share a gravitational association with Capella, even though the two are separated by nearly 15°, equivalent to a distance of 5.9 parsecs.
Reader's Guide
50 Persei's significance lies in its multiple variable star classifications and its role as a candidate Gamma Doradus variable, a class of pulsating stars. The subsequent reclassification by an automated program as both an RS Canum Venaticorum and a BY Draconis variable highlights the complexity of stellar variability and the challenges of automated classification. Its probable binary nature and physical association with the HIP 19255 system, with orbital timescales spanning hundreds to millions of years, provide insight into hierarchical stellar systems. The detection of an infrared excess at 70 μm suggests the presence of a circumstellar debris disk, indicating ongoing planetary system formation or evolution. The possible gravitational association with Capella, despite the large angular separation, adds to the star's context within the local stellar neighborhood. These combined characteristics make 50 Persei a valuable object for studying stellar pulsation, binary dynamics, and debris disk evolution.
Did You Know?
- 50 Persei has an apparent magnitude of 5.52, visible to the naked eye.
- The star emits an infrared excess at 70 μm, indicating a circumstellar debris disk.
- It is probably a binary system with an unseen companion and is physically associated with HIP 19255.
More in Variable Stars, Part 7 1-24
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