CE Gruis

Short description: Binary star system in the constellation Grus

CE Gruis

A visual band light curve for CE Gruis, adapted from Tuohy et al. (1987)[1]

Observation data
Equinox J2000.0]] (ICRS)
Constellation | Grus
Right ascension |  21h 37m 56.38s[2]
Declination | −43° 42′ 13.1″[2]
Apparent magnitude (V) | ~18[3]
Characteristics
Variable type | AM Her[2]
Details
White dwarf
Mass| ~1.0[4] M☉
Other designations

Gru V1[5]

Database references
SIMBAD| data

CE Gruis is a faint binary star system in the constellation Grus. It is a variable star, with a B-band brightness that ranges from a peak magnitude of 17.4 down to a minimum of 19.5[6] over a period of 108.6 minutes.[7] The system is composed of a white dwarf and donor star, locked into a close, synchronous orbit. In such systems, known as polars, material from the donor star does not form an accretion disc around the white dwarf because of its intense magnetic field, but rather streams directly onto it along columns.[4]

This was first identified as a system of interest by M. R. S. Hawkins in 1983 as part of a survey of faint variable objects in the Grus constellation. Catalogued as Grus V-1, it was found to show a high degree of variability as well as an intense emission of ionized helium. These properties suggested it may be a cataclysmic variable of the AM Herculis type. The binary period of 108.6 minutes lay within the range of 100–115 minute periods that a majority of known AM Her systems displayed. The system's emission pattern shows a blue and red component that is characteristic of cyclotron emission from accretion tunnels along a dipolar axis. Finally, the repeating modulation of the variability didn't match the erratic pattern observed with accretion disks.[3]

In 1990, strong circular polarization was observed coming from this system, which confirmed its identity as a polar. The cyclotron emission is coming from two regions on the surface of the white dwarf; the first polar to have two emission regions identified. The so-called 'blue pole' is visible throughout the orbit and thus is located on the hemisphere above the orbital plane. In contrast, the 'red pole' is eclipsed by the white dwarf for about 70% of the orbit. However, the red pole is likely the dominant emission region on the surface. The emission regions are linearly extended and lie at 30° offsets from the magnetic poles. They are nearly aligned with the axis of rotation.[8]

X-ray emissions were first detected from this system in 2002 as part of a survey of polars by the XMM-Newton space observatory. The X-ray spectrum must be fitted using a shock-based model caused by a sudden change in acceleration; there are no soft X-rays that are seen on other polars, possibly as a result of blobby accretion. The white dwarf has an estimated mass about equal to the mass of the Sun.[4]

## References

1. ↑ Tuohy1987, Ian R.; Ferrario, Lilia; Wickramasinghe, D. T.; Hawkins, M. R. S. (1987). "2.3 metre multi-colour photometry of a new AM Herculis variable". Publications of the Astronomical Society of Australia 7 (1): 60–64. doi:10.1017/S1323358000021858. Bibcode: 1987PASA....7...60T. https://www.cambridge.org/core/journals/publications-of-the-astronomical-society-of-australia/article/abs/23-metre-multicolour-photometry-of-a-new-am-herculis-variable/8D87E79B08B4859E4E8510001B18EC8E. Retrieved 9 January 2022.
2. ↑ 2.0 2.1 2.2 Downes, Ronald et al. (April 1997). "A Catalog and Atlas of Cataclysmic Variables". Publications of the Astronomical Society of the Pacific 109: 345–440. doi:10.1086/133900. Bibcode: 1997PASP..109..345D.
3. ↑ 3.0 3.1 Tuohy, Ian R. et al. (May 1988). "Evidence for Nonpolar Emission in a New AM Herculis Candidate". Astrophysical Journal Letters 328: L59. doi:10.1086/185160. Bibcode: 1988ApJ...328L..59T.
4. ↑ 4.0 4.1 4.2 Ramsay, Gavin; Cropper, Mark (2002). "First X-ray Observations of the Polar CE Gru". Monthly Notices of the Royal Astronomical Society 335 (4): 918–22. doi:10.1046/j.1365-8711.2002.05666.x. Bibcode: 2002MNRAS.335..918R.
5. ↑ "CE Gru". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=CE+Gru.
6. ↑ Samus, N. N. et al. (2009). General Catalogue of Variable Stars (Samus+ 2007-2013). 1. Bibcode: 2009yCat....102025S.
7. ↑ Downes, Ronald A. et al. (2001). "A Catalog and Atlas of Cataclysmic Variables: The Living Edition". Publications of the Astronomical Society of the Pacific 113 (784): 764. doi:10.1086/320802. Bibcode: 2001PASP..113..764D.
8. ↑ Wickramasinghe, D. T. et al. (July 1991). "Two-pole emission in Grus V 1". Monthly Notices of the Royal Astronomical Society 251: 137. doi:10.1093/mnras/251.1.137. Bibcode: 1991MNRAS.251..137W.

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Constellation of Grus

* List of stars in Grus
* List of star names in Grus
* Grus in Chinese astronomy

Stars|

| Bayer|

* α (Alnair)
* β (Tiaki)
* γ (Aldhanab)
* δ1
* δ2
* ε
* ζ
* η
* θ
* ι
* κ
* λ
* μ1
* μ2
* ν
* ξ
* ο
* π1
* π2
* ρ
* σ1
* σ2
* τ1
* τ2
* τ3
* υ
* φ

|

Variable|

* S
* U
* W
* RS
* RZ
* BC
* BP
* BZ
* CE
* DL
* DQ

HR|

* 8236
* 8241
* 8299
* 8323
* 8366
* 8379
* 8440
* 8477
* 8484
* 8501
* 8635
* 8639
* 8657
* 8658
* 8659
* 8685
* 8713
* 8749
* 8760
* 8771
* 8791
* 8793
* 8814
* 8835
* 8846
* 8847
* 8877
* 8896
* 8898

HD|

* 208487
* 213240
* 215456

Other|

* 2MASS J22282889–4310262
* Gliese 832
* GJ 4248
* PSR J2144−3933
* S5-HVS1
* WASP-95
* WISE 2220−3628

| Exoplanets|

* Gliese 832 b
* c
* HD 208487 b
* HD 213240 b
* Tau1 Gruis b

|

Galaxies|

| NGC|

* 7070
* 7070A
* 7072
* 7075
* 7079
* 7087
* 7091
* 7097
* 7107
* 7117
* 7118
* 7119
* 7144
* 7145
* 7162
* 7166
* 7169
* 7213
* 7232
* 7233
* 7249
* 7297
* 7299
* 7307
* 7322
* 7334
* 7355
* 7368
* 7382
* 7400
* 7404
* 7410
* 7412
* 7418
* 7421
* 7424
* 7456
* 7462
* 7470
* 7476
* 7496
* 7531
* 7545
* 7552
* 7582
* 7590
* 7599
* 7632
* 7658

|

Other|

* IC 1459
* IC 5201

| Galaxy clusters|

* Abell S1063

|

Category

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