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VY Canis Majoris

Size comparison between the Sun and VY Canis Majoris
Dữ liệu quan sát
Kỷ nguyên J2000      Xuân phân J2000
Chòm sao Canis Major
Xích kinh 07h 22m 58.33s[1]
Xích vĩ −25° 46′ 03.17″[1]
Cấp sao biểu kiến (V) 7.9607[2]
Các đặc trưng
Kiểu quang phổM3[1]-M5e Ia[3]
Chỉ mục màu B-V2.24[1]
Kiểu biến quangSemiregular[4]
Trắc lượng học thiên thể
Vận tốc xuyên tâm (Rv)49 ± 10[1] km/s
Chuyển động riêng (μ) RA: 9.84[1] mas/năm
Dec.: 0.75[1] mas/năm
Thị sai (π)1.78 ± 3.54[1] mas
Khoảng cách~4,900 ly
(~1,500[5] pc)
Chi tiết
Khối lượng~15[6]-25[7] M☉
Bán kính~600-2,600[8] R☉
Độ sáng~2-5.6×105[9][10] L☉
Nhiệt độ~3000[10] K
Tên gọi khác

VY Canis Majoris (VY CMa) is a red hypergiant star located in the constellation Canis Major. At between 1800 and 2100 solar radii (approx 2,500,000,000 to 2,900,000,000 km across or 1,550,000,000 to 1,800,000,000 miles), it is the largest known star and also one of the most luminous known. It is located about 1.5 kiloparsecs (4.6×1016 km) or about 4,900 light years away from Earth. Unlike most hypergiant stars, which occur in either binary or multiple star systems, VY CMa is a single star. It is categorized as a semiregular variable and has an estimated period of 2000 days.[4]

Nature of VY Canis Majoris[sửa | sửa mã nguồn]

The first known record of VY Canis Majoris is in the star catalogue of Jérôme Lalande, on March 7, 1801. The catalogue listed VY CMa as a 7th magnitude star. Further studies on its apparent magnitude during the 19th century showed that the star has been fading since 1850.[11]

Since 1847, VY CMa has been known to be a red star.[11] During the 19th century, observers measured at least six discrete components to VY CMa, suggesting the possibility that it is a multiple star. These discrete components are now known to be bright areas in the surrounding nebula. Visual observations in 1957 and high-resolution imaging in 1998 showed that VY CMa does not have a companion star.[6][11]

VY CMa is a high-luminosity M star with an effective temperature of about 3,000 K, placing it at the upper-right hand corner of the Hertzsprung–Russell diagram and suggesting that it is a highly evolved star. During its main sequence, it would have been an O star[10] with a mass of about 30 to 40 M☉.[6]

Measuring the distance[sửa | sửa mã nguồn]

Stellar distances can be calculated by measuring parallaxes as the Earth orbits around the Sun. However, VY CMa has a tiny parallax with a high margin of error, which makes it unreliable to calculate its distance using this method.[12]

In 1976, Charles J. Lada and Mark J. Reid published the discovery of a bright-rimmed molecular cloud 15 minutes of arc east of VY CMa. At the edge of the cloud bordered by the bright rim, an abrupt decrease in the CO emission and an increase in brightness of the 12CO emission were observed, indicating possible destruction of molecular material and enhanced heating at the cloud-rim interface, respectively. Lada and Reid assumed the distance of the molecular cloud is approximately equal to that of the stars, which are members of open cluster NGC 2362, that ionize the rim. NGC 2362 has a distance of 1.5 ± 0.5 kiloparsecs as determined from its color-magnitude diagram.[10]

VY CMa is projected onto the tip of the rim, suggesting its association with the molecular cloud. In addition to that, the velocity of the molecular cloud is very close to the velocity of the star. This further indicates the association of the star with the molecular cloud, and consequently with NGC 2362, which means VY CMa is also at a distance of 1.5 kpc.[5]

Size[sửa | sửa mã nguồn]

Right to left: VY Canis Majoris compared to Betelgeuse, Rho Cassiopeiae, The Pistol Star and the Sun (not visible in this thumbnail). The orbits of Jupiter and Neptune are also shown.
Relative sizes of the planets in the Solar System and several well known stars, including VY Canis Majoris.
1. Mercury < Mars < Venus < Earth
2. Earth < Neptune < Uranus < Saturn < Jupiter
3. Jupiter < Wolf 359 < Sun < Sirius
4. Sirius < Pollux < Arcturus < Aldebaran
5. Aldebaran < Rigel < Antares < Betelgeuse
6. Betelgeuse < Mu Cephei < VV Cephei A < VY Canis Majoris.

VY Canis Majoris is the largest known star.

University of Minnesota professor Roberta M. Humphreys estimates the radius of VY CMa at 1,800 to 2,100 solar radii.[8] To illustrate, if Earth's Sun were replaced by VY Canis Majoris, its radius might extend beyond the orbit of Saturn (about 9 AU). Assuming the upper size limit of 2100 solar radii, light would take more than 2.7 hours to travel around the star's circumference, compared to 14.5 seconds for the Sun. It would take 7×1015 Earths to fill the volume of VY Canis Majoris. [13]


If the Earth were to be represented by a sphere one centimeter in diameter, the Sun would be represented as a sphere with a diameter of 109 centimeters, at a distance of 117 meters. At these scales, VY Canis Majoris would have a diameter of approximately 2.3 kilometers, assuming the upper limit estimate of its radius.

Luminosity[sửa | sửa mã nguồn]

In 2006, Humphreys used the spectral energy distribution and distance of VY CMa to calculate its luminosity. Since most of the radiation coming from the star is reprocessed by the dust in the surrounding cloud, she integrated the total fluxes over the entire nebula and showed that VY CMa has a luminosity of 4.3×105 L☉.[8]

Controversy[sửa | sửa mã nguồn]

VY Canis Majoris ejects huge amounts of gas during its outbursts. Credit: NASA, ESA, and R. Humphreys (University of Minnesota)[14]

There are two conflicting opinions of the properties of VY CMa. In one view[8], the star is a very large and very luminous red hypergiant. In another opinion (such as Massey, Levesque, and Plez's study[15]), the star is a normal red supergiant, with a radius around 600 solar radii. In this case, its surface would extend well past the orbit of Mars in comparison to our solar system.

Like its size, the luminosity of VY CMa is also the subject of doubt. Humphreys contests that visual photometry is not sufficient for stars with enough circumstellar dust to reprocess the visual and red fluxes into the thermal infrared.[8]

See also[sửa | sửa mã nguồn]

References[sửa | sửa mã nguồn]

  1. ^ a b c d e f g h “SIMBAD basic query result: VY Canis Majoris”. SIMBAD, Centre de Données astronomiques de Strasbourg. Truy cập ngày 7 tháng 3 năm 2009.
  2. ^ a b “Hipparchos catalogue: query form”. CASU Astronomical Data Centre. Cambridge Astronomical Survey Unit. 2006. Truy cập ngày 10 tháng 3 năm 2009.
  3. ^ a b Lipscy, S. J.; Jura, M.; Reid, M. J. (10 tháng 6 năm 2005). “Radio photosphere and mass-loss envelope of VY Canis Majoris”. The Astrophysical Journal. The American Astronomical Society. 626: 439–445.
  4. ^ a b Monnier, J. D.; Geballe, T. R.; Danchi, W. C. (1 tháng 8 năm 1998). “Temporal variations of midinfrared spectra in late-type stars”. The Astrophysical Journal. American Astronomical Society. 502: 833–846.
  5. ^ a b Lada, C. J.; Reid, M. (tháng 3 năm 1976). “The discovery of a molecular cloud associated with VY CMa”. Bulletin of the American Astronomical Society. American Astronomical Society. 8: 322.
  6. ^ a b c Wittkowski, M.; Langer, N.; Weigelt, G. (27 tháng 10 năm 1998). “Diffraction-limited speckle-masking interferometry of the red supergiant VY CMa”. Astronomy and Astrophysics. European Southern Observatory. 340: 39–42.
  7. ^ Monnier, J. D.; Danchi, W. C.; Hale, D. S.; Lipman, E. A.; Tuthill, P. G.; Townes, C. H. (10 tháng 11 năm 2000). “Mid-infrared interferometry on spectral lines. II. Continuum (dust) emission around IRC +10216 and VY Canis Majoris”. The Astrophysical Journal. The American Astronomical Society. 543: 861–867.
  8. ^ a b c d e Humphreys, Roberta (13 tháng 10 năm 2006). VY Canis Majoris: the astrophysical basis of its luminosity. Truy cập ngày 15 tháng 5 năm 2007. Đã bỏ qua tham số không rõ |booktitle= (trợ giúp)
  9. ^ Monnier, J. D.; Tuthill, P. G.; Lopez, B.; Cruzalebes, P.; Danchi, W. C.; Haniff, C. A. (10 tháng 2 năm 1999). “The last gasps of VY Canis Majoris: aperture synthesis and adaptive optics imagery”. The Astrophysical Journal. American Astronomical Society. 512: 351–361. doi:10.1086/306761.
  10. ^ a b c d Lada, Charles J.; Reid, Mark J. (1 tháng 1 năm 1978). “CO observations of a molecular cloud complex associated with the bright rim near VY Canis Majoris”. The Astrophysical Journal. American Astronomical Society. 219: 95–104.
  11. ^ a b c Robinson, L. J. (7 tháng 12 năm 1971). “Three somewhat overlooked facets of VY Canis Majoris”. Commission 27 of the I. A. U., Information Bulletin on Variable Stars. Konkoly Observatory, Budapest (599).
  12. ^ Pogge, Richard W. (31 tháng 10 năm 2006). “Stellar distances”. Astronomy 162: Introduction to Stars, Galaxies and the Universe. Ohio State University. Truy cập ngày 20 tháng 3 năm 2009.
  13. ^ Volume with radius 9.58 AU=1.23×1037 m³; Earth volume 1.08×1021 m³; ratio is 1.14×1016 or 11.4 quadrillion.
  14. ^ HubbleSite: Astronomers Map a Hypergiant Star's Massive Outbursts
  15. ^ Massey, Philip; Levesque, Emily M.; Plez, Bertrand (1 tháng 8 năm 2006). “Bringing VY Canis Majoris down to size: an improved determination of its effective temperature”. The Astrophysical Journal. American Astronomical Society. 646: 1203–1208. doi:10.1086/505025. Liên kết ngoài trong |title= (trợ giúp)

Further reading[sửa | sửa mã nguồn]

  • Kastner, Joel H. (1998). “Hubble Space Telescope Imaging of the Mass-losing Supergiant VY Canis Majoris”. Astronomical Journal. 115 (4): 1592–1598. doi:10.1086/300297. Đã bỏ qua tham số không rõ |coauthors= (gợi ý |author=) (trợ giúp); Chú thích có tham số trống không rõ: |month= (trợ giúp)

External links[sửa | sửa mã nguồn]

Tọa độ: Sky map 07h 22m 58.33s, −25° 46′ 03.17″

vi:VY Canis Majoris

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