NML Cygni

NML Cygni

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′ 59.4″[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)	12.3[6]
Apparent magnitude (B)	18.64
Apparent magnitude (V)	16.60
Apparent magnitude (G)	11.0330
Apparent magnitude (J)	4.877
Apparent magnitude (H)	2.389
B−V color index	+2.04[2]
Variable type	SRc[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	40[7] M☉
Luminosity	229,000+40,000 −41,000[8] L☉
Temperature	3,300[3] K
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 by radius, 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.

The distance of NML Cygni from Earth is estimated to be around 1.6 kpc, about 5,300 light-years.^[9] 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.^[10]

The radius of NML Cyg is uncertain but it was given calculations between 1,183 and 2,770 times that of the Sun (R_☉). If placed at the center of the Solar System, its surface would potentially extend past the orbit of Jupiter or Saturn.

Observational history

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.^[12] The name NML comes from the names of these three discoverers.^[13] The second star was briefly referred to as NML Tauri^[14] but is now known as IK Tauri,^[15] an M9 Mira variable. NML Cygni has since also been given the designation V1489 Cygni on account of the small semi-regular brightness variations,^[16] 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.^[17] H
₂O, SiO, CO, HCN, CS, SO, SO
₂, and H
₂S molecules have also been detected.^[18]

Physical characteristics

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.^[5][10] 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

The bolometric luminosity (L_bol) 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.^[19][20][21] 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.^[22] 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.^[a][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.^[23]

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] Estimates of its current mass are difficult, but it is expected to be somewhere around 40 M_☉.^[7]

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][10] and it exhibits a bean-shaped asymmetric nebula that is coincident with the distribution of its H₂O vapor masers.^[24]

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.^[25] These dust envelopes are formed due to the strong post-main-sequence wind, which has a velocity 23 km/s.^[10]

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.^[10]

See also

• UY Scuti
• Westerlund 1 W26

Notes

References

This page was last edited on 22 March 2024, at 20:37