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Details for Revision 1
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Name |
BX Mon |
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AAVSO UID |
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Constellation |
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J2000.0 |
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B1950.0 |
07 22 52.94 -03 29 51.3 |
Galactic coord. |
220.035 +5.881 |
Other names

(Internal only)
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Please note that aliases shown in grey link to obsolete records.
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AAVSO 0720-03 |
ASAS J072523-0335.9 |
EM* AS 150 |
HV 10446 |
MHA 61-12 |
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Variability type |
* |
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Spectral type |
M4ep+F0II-III |
Mag. range |
9.5 - 13.4 p |
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Discoverer |
-- |
Epoch |
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Outburst |
-- |
Period |
1374 d (3.76 y) |
Rise/eclipse dur. |
39% (77 weeks) |
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Remarks
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Some references may be clicked to view in new window. Roll over index number to view submission details.
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1 |
Admin, VSX
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Before 1940 the dominant period was 1373 d, a beat period of the orbital period of 1256 days and the rotation period of 656 days of the M giant. |
2 |
GCVS Team |
Usually was considered as mira type variable [M.W.Mayall, HB N913, 1940.]. In the Table the epoch of light maximum and the period are given according to [H. van Schewick, BZ 24, 113, 1942.]. According to [P.A.Whitelock, R.M.Catchpole, IBVS N2296, 1983.] the Balmer emission lines originate in the nebulosity surrounding the symbiotic system and are excited by the hot component, and light variations are due to the orbital motion in the system. |
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References
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Click reference title/citation to view in new window. Roll over index number to view submission details.
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1 |
M. Gromadzki, J. Mikolajewska, I. Soszynski, 2013, arXiv:1312.6063 [astro-ph.SR] |
2013arXiv1312.6063G |
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E.M. Leibowitz, L. Formiggini, 2011, arXiv:1102.4458v1 [astro-ph.SR] |
2011arXiv1102.4458L |
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G.Pojmanski, Acta Astronomica 52, 397, 2002. |
2002AcA....52..397P |
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P.A.Whitelock, R.M.Catchpole, IBVS N2296, 1983. |
1983IBVS.2296....1W |
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V.P.Zessewitsch, M.S.Kazanasmas, Atlas of Finding Charts for Variable Stars, M., 1971. |
1971afcv.book.....T |
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External Links
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Supporting Documents
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Revision History
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Currently approved revision is checked. Click revision number to view details of that revision.
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