X Per
Observer: GDAA
Spectrum Data
FITS Header Metadata
Show FITS Header
| Key | Value |
|---|---|
| SIMPLE | True |
| BITPIX | -32 |
| NAXIS | 1 |
| NAXIS1 | 2765 |
| CRPIX1 | 1 |
| CDELT1 | 1.44606267595084 |
| CRVAL1 | 3801.89575195313 |
| CTYPE1 | Wavelength |
| CUNIT1 | Angstrom |
| SWCREATE | RSpec 2.1.1.18 |
| VERSION | RSpec 2.1.1.18 |
| OBSERVER | HLAD |
| BSS_SITE | Sandvreten Observatory L11 |
| BSS_INST | T41 |
| OBJNAME | X Per |
| DATE-OBS | 2025-12-17T18:21:19 |
| EXPTIME | 900 |
| BSS_VHEL | 0 |
FITS Spectral Image
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Calibrated Spectrum
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Observation Image
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Metadata
| Field | Value |
|---|---|
| Object Name | X Per |
| Observer | GDAA |
| Site | Legacy Site (update me) |
| Equipment | Legacy Equipment (update me) |
| Observation Date | 2025-12-23 23:30 |
| Julian Date | 2461033.47982 |
| Created | 2025-12-23 23:30 |
| Updated | 2025-12-24 12:07 |
Notes
The conventional star component of X Persei has been classified either as an O-type giant or a B-type main sequence star. It is a Be star, rotating rapidly, and at times surrounded by a disk of expelled material. This qualifies it as a Gamma Cassiopeiae variable, and the visual range is magnitude 6 - 7. In 1989 and 1990, the spectrum of X Persei changed from a Be star to a normal B class star while it faded significantly. This appears to have been caused by the loss of the excretion disk. The disk has since reformed and shows strong emission lines.[9] (Wiki)