RW Cephei
CHARA/MIRC-X image of RW Cephei in the H-band during the "great dimming", revealing a box-like shape and a dark patch on the western side of the star
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cepheus
Right ascension 22h 23m 07.01521s[1]
Declination +55° 57′ 47.6244″[1]
Apparent magnitude (V) +6.65[2] (6.0–7.6[3])
Characteristics
Evolutionary stage Red or yellow hypergiant
Spectral type K2 0-Ia[4] (G8 - M2Ia-0[3])
Apparent magnitude (K) 1.88[2]
U−B color index 2.38[2]
B−V color index 2.22[2]
Variable type SRd[5]
Astrometry
Radial velocity (Rv)−56.00[6] km/s
Proper motion (μ) RA: −3.606[1] mas/yr
Dec.: −2.881[1] mas/yr
Parallax (π)0.1140 ± 0.0342 mas[1]
Distance3,400+220
−200 pc[7][8]
Absolute magnitude (MV)−8.0[9] – −9.4[10]
Details
Radius900–1,760,[11] 940[8][lower-alpha 1] R☉
Luminosity300,000[8] L☉
Surface gravity (log g)0.2[12] cgs
Temperature4,200[11]–4,400,[8] 3,900[11] (during the dimming) K
Metallicity [Fe/H]+0.17±0.20[13] dex
Other designations
HD 212466, HIP 110504, SAO 34387, BD+55°2737, AAVSO 2219+55A
Database references
SIMBADdata

RW Cephei is a K-type hypergiant and a semirregular variable star in the constellation Cepheus, at the edge of the Sharpless 132 H II region and close to the small open cluster Berkeley 94. It is among the largest stars known with a radius of almost 1,000 times that of the Sun (R☉), nearly as large as the orbit of Jupiter.

In 2022, the star underwent a "great dimming" event similar to Betelgeuse.

The temperature intermediate between the red supergiants and yellow hypergiants has led to it being variously considered as a red hypergiant[14][15] or yellow hypergiant.[16][17]

Observational history

The first documented sighting of RW Cephei dates back to 1746 when it was included in a star catalog compiled by James Bradley.[18] It has been described as a red star since at least the 1840s,[lower-alpha 2] when Friedrich Wilhelm Argelander noted it as "very red" in his catalog.[19] RW Cephei was independently discovered to be variable by Thomas William Backhouse and Henrietta Swan Leavitt in 1899 and 1907 respectively,[20][21] but has been suspected to be variable by Angelo Secchi since at least 1868.[22] The star was designated RW in 1908, being the fifteenth discovered variable in Cepheus.[23] Analysis of spectra in 1942 revealed RW Cephei to be a highly luminous hypergiant star, appearing more luminous than Mu Cephei.[24] More detailed spectral studies in 1956 and 1972 revealed unique spectral features,[25][26] setting it apart from the other known hypergiants.[26] Since then, the star has been studied infrequently over the decades. In late 2022, RW Cephei was announced to be undergoing a great dimming event,[15][27][28] and it was subsequently observed by the CHARA interferometry array in December.[11]

Distance

The distance to RW Cephei has been estimated on the basis of its spectroscopic luminosity and it is assumed to be a member of the Cepheus OB1 association, placing it within the Perseus Arm of the Milky Way.[29] The Gaia Data Release 2 and Gaia Early Data Release 3 parallaxes lead to distance estimates of 3,416+1,366
−829 pc[30] and 6,666+1,561
−1,006 pc[31] respectively. Cepheus OB1 is generally considered to be at about 3,400 pc.[7] The open cluster Berkeley 94, of which RW Cephei may be a member, is thought to be at a distance of 3,900±110 pc.[14] The star and cluster are part of the larger star-forming region Sh 2-132.[32]

Variability

A light curve for RW Cephei, plotted from Hipparcos data[33]

The magnitude range of RW Cephei was given as 8.2–8.8 using photographic plates in the initial report,[21] while later studies found the photographic range to be from 8.6–10.7,[34][5] noting that maxima and minima cannot be derived with any certainty.[34] Other authors estimate an amplitude of only around 0.5 magnitudes.[35] Modern estimates put the range of variability from 6.0 to 7.6 in the V-band.[3]

RW Cephei has been classified as a semi-regular variable star of type SRd, meaning that it is a slowly varying yellow giant or supergiant. The General Catalogue of Variable Stars cites a 1952 study giving a period of approximately 346 days,[34][5] while other studies suggest different periods and certainly no strong periodicity.[36]

Great dimming

Comparison of CHARA array images taken on December 2022 and July 2023, showing the dimming and subsequent rebrightening of RW Cephei

In December of 2022, the star was reported by two astronomers to be going through a "great dimming", reaching a fainter than usual magnitude of 7.6.[15][27][28] It was speculated to be caused by short periods of enhanced mass loss leading to the condensation of dust that partially obscures the stellar photosphere.[8] This was later confirmed by observations with the CHARA array, revealing a dark patch on the western side of the star suggested to be a dust cloud released in a recent surface mass ejection.[11] An unusually bright maximum attained in 2019 right before the dimming was suspected to be caused by an energetic convective upwelling of hot gas, later being expelled and cooling into a dust cloud obscuring the star.[11] The event is compared to the great dimming of Betelgeuse that happened in late 2019[8][11][15][27][28] and the dimming events seen in the historical light curve of VY Canis Majoris.[8][11]

Spectra taken by an amateur astronomer show the appearance of several new emission lines during the dimming, most notably H-α and the K I lines at 766.5 and 769.9 nm.[17] The H-α line is blueshifted by ~40 km/s relative to the star, suggesting the source of the emission is expanding outwards.[17]

Previous observations using photographic plates taken between 1948 and 1951 reveal a similar dimming from magnitude 9.16 down to 9.5, followed by a rapid re-brightening to magnitude 8.9.[37]

Spectrum

RW Cephei displays many complex lines in its spectrum, many of which are stronger and more broad than usual.[24][25][26] An initial study in 1956 focusing on the blue spectral region found many metal absorption lines with two components separated by a central maximum, attributed to emission superposed on an absorption line widened due to turbulence.[25] The shortward absorption components were found to be significantly stronger than the longward components, caused by an outward moving shell of gas.[25] A follow-up study in 1972 focusing on redder spectral regions found unusually strong Na D lines too intense to be caused by the interstellar medium.[26] The Fe I line was found to be 30% stronger than in normal K-type supergiants, while the Ti I and V I lines were of the same strength or weaker.[26] With these peculiar spectral features, the star finds no counterpart among the known hypergiants, with only Rho Cassiopeiae displaying remotely similar features.[26]

The spectrum has been classified as early as G8 and as late as M2, but it isn't clear that there has been actual variation. In the first MK spectral atlas, it was listed M0:Ia.[38] RW Cephei was later listed as the standard star for spectral type G8 Ia,[39] then as the standard for K0 0-Ia.[40] Based on the same spectra it was adjusted to the standard star for type K2 0-Ia.[41] Molecular bands characteristic of M-class stars are seen in infrared spectra, but not always in optical spectra.[42][43]

Physical properties

The temperature of RW Cephei is uncertain, with contradictory excitation strengths in the spectrum. A simple color correlation temperature fit gives temperatures around 3,749 K, while a full spectrum fit gives a temperature of 5,018 K.[12] Another fit using J-band spectral data and MARCS stellar models gives a temperature of 3,770±170 K.[13] This fit also results in a metallicity of [Fe/H] = +0.17±0.20, indicating the star is slightly metal-rich relative to the Sun.[13] A newer study finds a temperature of 4,400 K consistent with its spectral type.[8] Based on the CO line strength at 2.29 μm it is indicated that RW Cephei dropped in temperature from 4,200 K to 3,900 K during the dimming.[11]

Luminosities have been derived on the basis of a membership to Cepheus OB1, with studies finding exceptionally high luminosities of 545,000 L☉,[29] or 468,000 L☉.[44] A more recent study finds a somewhat lower luminosity of 300,000 L☉ using the spectral energy distribution of a DUSTY model fit.[8]

Imaging of RW Cephei by the CHARA array reveals the star to be box-like in shape. Images obtained using the SURFING algorithm result in a limb-darkened angular diameter of 2.45 mas, corresponding to a linear radius of 900–1,760 R☉ depending on the adopted distance.[11]

Surroundings

11.9 μm image of the extended emission around RW Cephei

The star shows evidence for a significant amount of circumstellar material in its spectrum.[26][45][8][11] The IRAS low resolution spectrum shows signatures of optically thick silicate emission at 10 and 18 μm,[46] an indication for high amounts of mass loss.[45] Emission in the first-overtone SiO bands was suspected in 1982,[47] and later confirmed using higher resolution spectra showing clear signs of emission at 4.0, 4.04 and 4.08 μm.[45] Direct imaging in mid-infrared bands reveals the source to be extended, having an azimuthally symmetric structure similar to IRC +10420.[48][8] The radius of this emission has been estimated to be ~0.3–0.4 arcseconds at 11.9 μm, corresponding to a physical radius of ~1,000–1,400 au at a distance of 3.4 kpc.[8]

Mass loss

The current mass loss rate of RW Cephei has been determined to be ~7×10−6 M☉/yr using a DUSTY model fit.[8] A previous study estimated 1.8×10−5 M☉/yr using silicate line strengths and adopting a distance of 2.8 kpc.[49] Analysis of the surrounding mid-infrared emission indicates that RW Cephei ended a period of enhanced mass loss ~95–140 years ago,[lower-alpha 3] suggesting that it has left the red supergiant phase and is currently evolving towards hotter temperatures.[8] The current mass loss phase appears to be dominated by several mass ejections, including the observed "great dimming".[8][11]

See also

Notes

  1. ↑ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
  2. ↑ The exact year of the observation is unknown, but it is believed to have been taken some time between 1841 and 1844
  3. ↑ Assuming a wind velocity of 50 km/s based on values for known red and yellow hypergiants

References

  1. 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 3 4 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
  3. 1 2 3 Watson, C. L. (2006). "The International Variable Star Index (VSX)". The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25. 25: 47. Bibcode:2006SASS...25...47W.
  4. ↑ Keenan, P. C.; Yorka, S. B. (1988). "1988 Revised MK Spectral Standards for Stars GO and Later". Bulletin d'Information du Centre de Données Stellaires. 35: 37. Bibcode:1988BICDS..35...37K.
  5. 1 2 3 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  6. ↑ Kharchenko, N. V.; Scholz, R.-D.; Piskunov, A. E.; Röser, S.; Schilbach, E. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ˜55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889. arXiv:0705.0878. Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776. S2CID 119323941.
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  9. ↑ Stencel, Robert E.; Pesce, Joseph E.; Hagen Bauer, Wendy (1988). "Far-infrared circumstellar 'debris' shell of red supergiant stars". Astronomical Journal. 95: 141. Bibcode:1988AJ.....95..141S. doi:10.1086/114622.
  10. ↑ Humphreys, R. M. (1984). "The brightest stars in the Magellanic Clouds and other late-type galaxies". IAU Symposium. 108: 145–156. Bibcode:1984IAUS..108..145H. doi:10.1017/S0074180900040134.
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  16. ↑ Castro-Carrizo, A.; Quintana-Lacaci, G.; Bujarrabal, V.; Neri, R.; Alcolea, J. (2007). "Arcsecond-resolution 12CO mapping of the yellow hypergiants IRC +10420 and AFGL 2343". Astronomy and Astrophysics. 465 (2): 457–467. arXiv:astro-ph/0702400. Bibcode:2007A&A...465..457C. doi:10.1051/0004-6361:20066169. S2CID 53127885.
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  22. ↑ Secchi, Angelo (1868). Sugli spettri prismatici delle stelle fisse. Bibcode:1868sspd.bookR....S.
  23. ↑ Dunér, Nils Christofer; Hartwig, Ernst; Müller, G. (October 1908). "Benennung von neu entdeckten veränderlichen Sternen". Astronomische Nachrichten. 179 (6): 85. Bibcode:1908AN....179...85D. doi:10.1002/asna.19081790602. ISSN 0004-6337.
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  26. 1 2 3 4 5 6 7 Gahm, G. F.; Hultqvist, L. (1972). "Spectral properties of luminous late-type stars". Astronomy and Astrophysics. 16: 329. Bibcode:1972A&A....16..329G. ISSN 0004-6361.
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  30. ↑ Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Mantelet, G.; Andrae, R. (2018). "Estimating Distance from Parallaxes. IV. Distances to 1.33 Billion Stars in Gaia Data Release 2". The Astronomical Journal. 156 (2): 58. arXiv:1804.10121. Bibcode:2018AJ....156...58B. doi:10.3847/1538-3881/aacb21. S2CID 119289017.
  31. ↑ Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (2021). "Estimating Distances from Parallaxes. V. Geometric and Photogeometric Distances to 1.47 Billion Stars in Gaia Early Data Release 3". The Astronomical Journal. 161 (3): 147. arXiv:2012.05220. Bibcode:2021AJ....161..147B. doi:10.3847/1538-3881/abd806. S2CID 228063812.
  32. ↑ Saurin, T. A.; Bica, E.; Bonatto, C. (2010). "Star clusters in the Sh2-132 complex: Clues about the connection between embedded and open clusters". Monthly Notices of the Royal Astronomical Society. 407 (1): 133. arXiv:1006.0246. Bibcode:2010MNRAS.407..133S. doi:10.1111/j.1365-2966.2010.16929.x. S2CID 53966692.
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  35. ↑ Rajchl, Rostislav (1933). "Observations d'etoiles variables". Publications of the Astronomical Institute of the Charles University. 18: 1–20. Bibcode:1933PAICU..18....1R.
  36. ↑ Percy, John R.; Kolin, David L. (2000). "Studies of Yellow Semiregular(SRd) Variables". The Journal of the American Association of Variable Star Observers. 28 (1): 1. Bibcode:2000JAVSO..28....1P.
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  38. ↑ Morgan, William Wilson; Keenan, Philip Childs; Kellman, Edith (1943). "An atlas of stellar spectra, with an outline of spectral classification". Chicago. Bibcode:1943assw.book.....M.
  39. ↑ Morgan, W. W.; Roman, Nancy G. (1950). "Revised Standards for Supergiants on the System of the Yerkes Spectral Atlas". Astrophysical Journal. 112: 362. Bibcode:1950ApJ...112..362M. doi:10.1086/145351.
  40. ↑ Morgan, W. W.; Keenan, P. C.; Abt, H. A.; Tapscott, J. W. (1981). "Some aspects of the spectroscopic behavior of the stars of highest luminosity in the region of the Hertzsprung gap". Astrophysical Journal. 243: 894. Bibcode:1981ApJ...243..894M. doi:10.1086/158654.
  41. ↑ Keenan, P. C.; Pitts, R. E. (1980). "Revised MK spectral types for G, K, and M stars". Astrophysical Journal Supplement Series. 42: 541. Bibcode:1980ApJS...42..541K. doi:10.1086/190662.
  42. ↑ McCuskey, S. W. (1955). "Stellar Spectra in Milky way REGIONS.III.A Region in Cepheus-Lacerta". Astrophysical Journal Supplement. 2: 75. Bibcode:1955ApJS....2...75M. doi:10.1086/190017.
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  44. ↑ de Jager, Cornelis (1998). "The yellow hypergiants". Astronomy and Astrophysics Review. 8 (3): 145–180. Bibcode:1998A&ARv...8..145D. doi:10.1007/s001590050009. ISSN 0935-4956. S2CID 189936279.
  45. 1 2 3 Rayner, John T.; Cushing, Michael C.; Vacca, William D. (December 2009). "The Infrared Telescope Facility (IRTF) Spectral Library: Cool Stars". The Astrophysical Journal Supplement Series. 185 (2): 289–432. arXiv:0909.0818. Bibcode:2009ApJS..185..289R. doi:10.1088/0067-0049/185/2/289. ISSN 0067-0049. S2CID 118500715.
  46. ↑ Simpson, Janet P. (February 1991). "IRAS Low-Resolution Spectral Observations of the 10 and 18 Micron Silicate Emission Features". The Astrophysical Journal. 368: 570. Bibcode:1991ApJ...368..570S. doi:10.1086/169721. ISSN 0004-637X.
  47. ↑ Rinsland, C. P.; Wing, R. F. (November 1982). "Observations of the first-overtone silicon monoxide bands in late-type stars". The Astrophysical Journal. 262: 201–212. Bibcode:1982ApJ...262..201R. doi:10.1086/160411. ISSN 0004-637X.
  48. ↑ Shenoy, Dinesh; Humphreys, Roberta M.; Jones, Terry J.; Marengo, Massimo; Gehrz, Robert D.; Helton, L. Andrew; Hoffmann, William F.; Skemer, Andrew J.; Hinz, Philip M. (March 2016). "Searching for Cool Dust in the Mid-to-far Infrared: The Mass-loss Histories of the Hypergiants μ Cep, VY CMa, IRC+10420, and ρ Cas". The Astronomical Journal. 151 (3): 51. arXiv:1512.01529. Bibcode:2016AJ....151...51S. doi:10.3847/0004-6256/151/3/51. ISSN 0004-6256. S2CID 119281306.
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