NML Cygni

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NML Cygni
NML Cygni SDSS DR9.jpg
NML Cygni, seen as the deep red star at the center, from the Sloan Digital Sky Survey DR9. Note the green circumstellar nebula surrounding the star.
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Cygnus
Right ascension 20h 46m 25.54s [1]
Declination +40° 06′ 59.5″ [1]
Apparent magnitude  (V)16.60 (variable) [2]
Characteristics
Evolutionary stage OH/IR [3] red hypergiant [4]
Spectral type M4.5–M7.9 Ia–III [5]
Apparent magnitude  (K)0.791±0.204 [1]
Apparent magnitude  (G)11.148 [1]
Apparent magnitude  (J)4.877±0.037 [1]
Apparent magnitude  (H)2.389±0.2 [1]
B−V color index +2.04 [2]
Variable type Semiregular variable star [6]
Astrometry
Proper motion (μ)RA: −1.55 [4]   mas/yr
Dec.: −4.59 [4]   mas/yr
Parallax (π)0.620 ± 0.047  mas [4]
Distance 5,250+420
−360  ly
(1,610+130
−110 [4]   pc)
Details
Mass 25 [4] (initial)  M☉
Radius <1,350+195
−229 [7] [a]   R☉
Luminosity 229,000+40,000
−41,000 [9]   L☉
Age 8 [4]   Myr
Other designations
NML Cyg, V1489  Cyg, RAFGL  2650, IRC  +40448, 2MASS  J20462554+4006594, AAVSO  2042+39
Database references
SIMBAD data

NML Cygni or V1489 Cygni (abbreviated to NML Cyg or V1489 Cyg) is a red hypergiant [4] or red supergiant (RSG) in the constellation Cygnus. It is possibly one of the largest known stars currently known, and is also possibly one of the most luminous and massive cool hypergiants, as well as one of the most luminous stars in the Milky Way.

Contents

The distance of NML Cygni from Earth is estimated to be around 1.6 kpc, about 5,300  light-years . [10] It is a part of the Cygnus OB2 association, one of the closest massive associations to the Sun, spanning nearly 2° on the sky or ~30 pc in radius at the distance of 1.74±0.2 kpc. [11] Based on the estimated distance and a measurement of its angular diameter of 7.8±0.64  milliarcseconds , [8] NML Cygni's physical radius is of 1,350  R☉. If placed at the center of the Solar System, its surface would potentially extend past the orbit of Jupiter.

Observational history

A near infrared (3.5 micron) light curve for V1489 Cygni, plotted from data published by Strecker (1975) V1489CygLightCurve.png
A near infrared (3.5 micron) light curve for V1489 Cygni, plotted from data published by Strecker (1975)

NML Cygni was discovered in 1965 by American astronomers Neugebauer, Martz, and Leighton who described two extremely red luminous stars, their colour being consistent with a black body temperature of 1,000 K. [13] The name NML comes from the names of these three discoverers. [14] The second star was briefly referred to as NML Tauri [15] but is now known as IK Tauri, [16] an M9 Mira variable. NML Cygni has since also been given the designation V1489 Cygni on account of the small semi-regular brightness variations, [17] but is still most commonly referred to as NML Cygni. Its composition began to be revealed with the discovery of OH masers (1612 MHz) in 1968. [18] H
2O , SiO , CO , HCN , CS , SO , SO
2 , and H
2S molecules have also been detected. [19]

Physical characteristics

H-alpha light image of Cygnus OB2, the stellar association in which NML Cygni is located CygOB2 med.jpg
H-alpha light image of Cygnus OB2, the stellar association in which NML Cygni is located

NML Cygni is an extremely large and luminous cool supergiant with parameters similar to that of another notable but more extreme cool hypergiant star, VY Canis Majoris, and is also known as a heavily mass-losing OH/IR supergiant. It is also a semiregular variable star with a period of either 1,280 or 940 days. [11] [5] It occupies the upper-right hand corner of the Hertzsprung–Russell diagram although most of the properties of the star depend directly on its distance.

Size, luminosity, and temperature

NML Cygni compared to the Sun and Earth orbit NML Cygni compared to the Sun and Earth orbit.png
NML Cygni compared to the Sun and Earth orbit

The bolometric luminosity (Lbol) for NML Cygni was originally calculated to be 500,000 L☉ at an assumed distance of 2  kpc and the radius was calculated to be 3,700 R☉ based on an 8.6  mas angular diameter and distance. [20] [21] [22] A 2006 study, similar to those conducted on VY Canis Majoris, suggests that NML Cygni is a normal red supergiant with consequently much lower luminosity and radius values. [23] More modern and accurate measurements give a distance around 1.6 kpc, which gives a luminosity around 200,000 L☉. A radio angular diameter of 44 mas was given based on the distance, suggesting the optical angular diameter may be around 22 mas. [4] This distance and a luminosity of 270,000 L☉ were combined with assumptions of the effective temperature of the star, giving a radius of 1,640 R☉ for a temperature of 3,250 K or possibly 2,770 R☉ for a temperature of 2,500 K. [b] [4] However, another paper gives a much lower radius of 1,183 R☉ based on an assumed effective temperature of 3,834 K and a lower distance of 1.22 kpc. [6] There is a Gaia Data Release 2 parallax for NML Cygni of 1.5259±0.5677  mas , but the underlying measurements show a considerable level of noise and the parallax is considered unreliable. [24]

NML Cygni's uniform disk angular diameter was measured by the CHARM2 survey, leading to an apparent size of 7.8±0.64  milliarcseconds . [8] Assuming the distance measured by Zhang et al. (2012) (1610+130
−110  parsecs ), [4] it leads to a physical radius of 1,350 R☉. [7] If placed in the center of the Solar System, its photosphere would past the orbit of Jupiter. NML Cygni is covered by a complex dust shell, so the measured angular diameter likely contain some parts of this disk, and therefore its physical radius may be smaller. [25]

Mass and mass loss

NML Cygni lies close to the expected position that a 25 M☉ star would evolve to after eight million years. [4]

NML Cygni is evolved and a number of heavy elements and molecules have been detected in its atmosphere, particularly oxygen, hydroxyl, and water. It is surrounded by dusty material [4] [11] and it exhibits a bean-shaped asymmetric nebula that is coincident with the distribution of its H2O vapor masers. [26]

NML Cygni has an estimated mass loss rate of 4.2 to 4.8×10−4 M☉ per year, [3] one of the highest known for any star. The annual parallax of NML Cygni is measured to be around 0.62 milliarcseconds. [4] From the observations, it is estimated that NML Cygni has two discrete optically thick envelopes of dust and molecules. The optical depth of the inner shell is found to be 1.9, whereas that of the outer one is 0.33. [27] These dust envelopes are formed due to the strong post-main-sequence wind, which has a velocity 23 km/s. [11]

Because of the star's position on the outskirts of the massive Cygnus OB2 association, the detectable effects of NML Cygni's radiation on the surrounding dust and gas are limited to the region away from the central hot stars of the association. [11]

See also

Notes

  1. ↑ Surrounding dusty region is very complex making the radius hard to determine. [8]
  2. ↑ Applying the Stefan-Boltzmann Law with a nominal solar effective temperature of 5,772  K:

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References

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  3. 1 2 Gordon, Michael S.; Humphreys, Roberta M.; Jones, Terry J.; Shenoy, Dinesh; Gehrz, Robert D.; Helton, L. Andrew; Marengo, Massimo; Hinz, Philip M.; Hoffmann, William F. (2018). "Searching for Cool Dust. II. Infrared Imaging of the OH/IR Supergiants, NML Cyg, VX SGR, S Per, and the Normal Red Supergiants RS per and T per". The Astronomical Journal. 155 (5): 212. arXiv: 1708.00018 . Bibcode:2018AJ....155..212G. doi: 10.3847/1538-3881/aab961 . S2CID   73650032.
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  7. 1 2 Lang, Kenneth R. (2006). Astrophysical formulae. Astronomy and astrophysics library. Vol. 1 (3rd ed.). Berlin: Springer. ISBN   978-3-540-29692-8.. The radius (R*) is given by:
  8. 1 2 3 Richichi, A.; Percheron, I.; Khristoforova, M. (2005-02-01). "CHARM2: An updated Catalog of High Angular Resolution Measurements". Astronomy & Astrophysics. 431 (2): 773–777. Bibcode:2005A&A...431..773R. doi:10.1051/0004-6361:20042039. ISSN   0004-6361. Data about NML Cygni is found here at VizieR.
  9. ↑ Davies, Ben; Beasor, Emma R. (March 2020). "The 'red supergiant problem': the upper luminosity boundary of Type II supernova progenitors". MNRAS . 493 (1): 468–476. arXiv: 2001.06020 . Bibcode:2020MNRAS.493..468D. doi: 10.1093/mnras/staa174 . S2CID   210714093.
  10. ↑ Schuster, Michael Thomas (2007). Investigating the Circumstellar Environments of the Cool Hypergiants. University of Minnesota. ISBN   978-0-549-32782-0.
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  13. ↑ Neugebauer, G.; Martz, D. E.; Leighton, R. B. (July 1965). "Observations of Extremely Cool Stars" (PDF). Astrophysical Journal . 142: 399–401. Bibcode:1965ApJ...142..399N. doi:10.1086/148300.
  14. ↑ Hearnshaw, J. B. (2 May 1996). "New infrared sources and their interpretation". The Measurement of Starlight: Two Centuries of Astronomical Photometry. Cambridge University Press. p.  278. ISBN   978-0-521-40393-1 . Retrieved 23 August 2012.
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  17. ↑ Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P. (27 November 1975). "61st Name-List of Variable Stars". Information Bulletin on Variable Stars . 1068 (1): 1. Bibcode:1975IBVS.1068....1K.
  18. ↑ Cohen, R. J.; Downs, G.; Emerson, R.; Grimm, M.; et al. (1 April 1987). "Narrow polarized components in the OH 1612-MHz maser emission from supergiant OH-IR sources". Monthly Notices of the Royal Astronomical Society . 225 (3): 491–498. Bibcode:1987MNRAS.225..491C. doi: 10.1093/mnras/225.3.491 . PMID   11540900.
  19. ↑ Marvel, Kevin (19 December 1996). "NML Cygni". The Circumstellar Environment of Evolved Stars As Revealed by Studies of Circumstellar Water Masers. Universal-Publishers. pp. 182–212. ISBN   978-1-58112-061-5 . Retrieved 23 August 2012.
  20. ↑ Zubko, Viktor; Li, Di; Lim, Tanya; Feuchtgruber, Helmut; Harwit, Martin (2004). "Observations of Water Vapor Outflow from NML Cygnus". The Astrophysical Journal. 610 (1): 427. arXiv: astro-ph/0405044 . Bibcode:2004ApJ...610..427Z. doi:10.1086/421700. S2CID   14352419.
  21. ↑ Monnier, J. D; Bester, M; Danchi, W. C; Johnson, M. A; Lipman, E. A; Townes, C. H; Tuthill, P. G; Geballe, T. R; Nishimoto, D; Kervin, P. W (1997). "Nonuniform Dust Outflow Observed around Infrared Object NML Cygni". The Astrophysical Journal. 481 (1): 420. arXiv: astro-ph/9702103 . Bibcode:1997ApJ...481..420M. doi:10.1086/304050. S2CID   9503967.
  22. ↑ Monnier, J. D.; Millan-Gabet, R.; Tuthill, P. G.; Traub, W. A.; Carleton, N. P.; Coude Du Foresto, V.; Danchi, W. C.; Lacasse, M. G.; Morel, S.; Perrin, G.; Porro, I. L.; Schloerb, F. P.; Townes, C. H. (2004). "High-Resolution Imaging of Dust Shells by Using Keck Aperture Masking and the IOTA Interferometer". The Astrophysical Journal. 605 (1): 436–461. arXiv: astro-ph/0401363 . Bibcode:2004ApJ...605..436M. doi:10.1086/382218. S2CID   7851916.
  23. ↑ Massey, Philip; Levesque, Emily M.; Plez, Bertrand (1 August 2006). "Bringing VY Canis Majoris down to size: an improved determination of its effective temperature". The Astrophysical Journal. 646 (2): 1203–1208. arXiv: astro-ph/0604253 . Bibcode:2006ApJ...646.1203M. doi:10.1086/505025. S2CID   14314968.
  24. ↑ Xu, Shuangjing; Zhang, Bo; Reid, Mark J.; Zheng, Xingwu; Wang, Guangli (2019). "Comparison of Gaia DR2 Parallaxes of Stars with VLBI Astrometry". The Astrophysical Journal. 875 (2): 114. arXiv: 1903.04105 . Bibcode:2019ApJ...875..114X. doi: 10.3847/1538-4357/ab0e83 . S2CID   119192180.
  25. ↑ Type of source (Bin, Cal, Com, Diam, UR)
  26. ↑ Schuster, Michael T.; Humphreys, Roberta M.; Marengo, Massimo (January 2006). "The Circumstellar Environments of NML Cygni and the Cool Hypergiants". The Astronomical Journal. 131 (1): 603–611. arXiv: astro-ph/0510010 . Bibcode:2006AJ....131..603S. doi:10.1086/498395. ISSN   0004-6256.
  27. ↑ DanchiI, W. C.; Green, W. H.; Hale, D. D. S.; McEleroy, K.; et al. (July 2001). "Proper Motions of Dust Shells Surrounding NML Cygni". The Astrophysical Journal . 555 (1): 405. Bibcode:2001ApJ...555..405D. doi: 10.1086/322237 .
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  29. Singh, A. P.; Edwards, J. L.; Humphreys, R. M.; Ziurys, L. M. (2021). "Molecules and Outflows in NML Cygni: New Insights from a 1 mm Spectral Line Survey". The Astrophysical Journal. 920 (2): L38. Bibcode:2021ApJ...920L..38S. doi: 10.3847/2041-8213/ac2c7c . S2CID   239023582.
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