Jump to content

Serpens

Coordinates: Sky map 17h 00m 00s, +03° 00′ 00″
This is a good article. Click here for more information.
From Wikipedia, the free encyclopedia

This is an old revision of this page, as edited by Legobot (talk | contribs) at 01:02, 19 August 2014 (Adding Good Article icon). The present address (URL) is a permanent link to this revision, which may differ significantly from the current revision.

Serpens
Constellation
Serpens CaputSerpens Cauda
List of stars in Serpens
AbbreviationSer
GenitiveSerpentis
Pronunciation/ˈsɜːrp[invalid input: 'ɨ']nz/,
genitive /sərˈpɛnt[invalid input: 'ɨ']s/
Symbolismthe Snake
Right ascensionSerpens Caput: 15h 10.4m to 16h 22.5m
Serpens Cauda: 17h 16.9m to 18h 58.3m
DeclinationSerpens Caput: 25.66° to −03.72°
Serpens Cauda: 06.42° to −16.14°
AreaSerpens Caput: 428 sq. deg.
Serpens Cauda: 208 sq. deg.
Total: 637 sq. deg. (23rd)
Main stars11
Bayer/Flamsteed
stars		57
Stars with planets15
Stars brighter than 3.00m1
Stars within 10.00 pc (32.62 ly)2
Brightest starα Ser (Unukalhai) (2.63m)
Messier objects2
Bordering
constellations		Serpens Caput:
Corona Borealis
Boötes
Virgo
Libra
Ophiuchus
Hercules

Serpens Cauda:
Aquila
Ophiuchus
Sagittarius
Scutum
Visible at latitudes between +80° and −80°.
Best visible at 21:00 (9 p.m.) during the month of July.

Serpens ("the Serpent", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the "Serpent-Bearer". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between μ Ser in Serpens Caput and ν Ser in Serpens Cauda.

The brightest star in Serpens is Unukalhai or Cor Serpentis "Serpent's Heart", with an apparent magnitude of 2.63. Part of the Milky Way passes through Serpens Cauda, which is therefore rich in deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Located in Serpens Caput are Seyfert's Sextet, one of the densest galaxy clusters known, and Arp 220, the prototypical ultraluminous infrared galaxy.

History

Serpens held by Ophiuchus, as depicted in Urania's Mirror, a set of constellation cards published in London c. 1825. Above the tail of the serpent is the now-obsolete constellation Taurus Poniatovii while below it is Scutum.

in Greek Mythology, Serpens represents a snake held by Asclepius, a healer. Asclepius, represented in the sky by the constellation Ophiuchus, which splits Serpens into two distinct halves, was known for killing a snake that was resurrected because a different snake had placed a certain herb on it before its "death". Serpens is depicted as either winding around Ophiuchus in the night sky or simply passing through him, although the precise reason for either of these is unknown.[1]

In some ancient atlases, the constellations Serpens and Ophiuchus were depicted as two separate constellations, although in most they were shown as a single constellation. Back in this time, there were no official constellation boundaries, so when depicted separately, their bodies were not intertwined with each other.[1]

In Chinese astronomy, most of the stars of Serpens represented part of a wall surrounding a marketplace, known as Tianshi, which was in Ophiuchus and part of Hercules. Serpens also contains a few Chinese constellations. Two stars in the tail represented part of Shilou, the tower with the market office. Another star in the tail represented Liesi, jewel shops. One star in the head (Mu Serpentis) marked Tianru, the crown prince's wet nurse, or sometimes rain.[1]

There were two "serpent" constellations in Babylonian astronomy, known as Mušḫuššu and Bašmu. It appears that Mušḫuššu was depicted as a hybrid of a dragon, a lion and a bird, and loosely corresponded to Hydra. Bašmu was a horned serpent (c.f. Ningishzida) and loosely corresponds to the Ὄφις constellation of Eudoxus of Cnidus on which the Ὄφις (Serpens) of Ptolemy is based.[2]

Characteristics

Serpens is unique among the 88 modern constellations in that it is split into two separate parts: Serpens Caput and Serpens Cauda, the head and tail respectively. The constellation is also one of the only ones that is dependent on another constellation for context; specifically, it is being held by the Serpent Bearer Ophiuchus.[1]

Serpens Caput is bordered by Libra to the south, Virgo and Boötes to the east, Corona Borealis to the north, and Ophiuchus and Hercules to the west; Serpens Cauda is bordered by Sagittarius to the south, Scutum and Aquila to the east, and Ophiuchus to the north and west. Covering 636.9 square degrees total, it ranks 23rd of the 88 constellations in size. It appears prominently in the both the northern and southern skies during the Northern Hemisphere's summer.[3] Its main asterism consists of 11 stars, and 108 stars in total are brighter than magnitude 6.5.[3]

Serpens Caput's boundaries, as set by Eugène Delporte in 1930, are defined by a 15-sided polygon, while Serpens Cauda's are defined by a 25-sided polygon. In the equatorial coordinate system, the right ascension coordinates of Serpens Caput's borders lie between 15h 10.4m and 16h 22.5m , while the declination coordinates are between 25.66° and −03.72°. Serpens Cauda's boundaries lie between right ascensions of 17h 16.9m and 18h 58.3m and declinations of 06.42° and −16.14°.[4] The International Astronomical Union (IAU) adopted the three-letter abbreviation "Ser" for the constellation in 1922.[5]

Notable features

The constellation Serpens (Caput) as it can be seen by the naked eye.

Stars

See also: List of stars in Serpens

Head stars

The brightest star in Serpens, Alpha Serpentis, or Unukalhai, is a red giant of spectral type K2III located approximately 22.68 parsecs (74.0 ly) away which marks the snake's heart. With a visual magnitude of 2.63,[6] it can easily be seen with the naked eye even in areas with substantial light pollution. A faint companion is in orbit around the red giant star,[7] although it is not visible to the naked eye. Located near Alpha is Lambda Serpentis, a magnitude 4.42 star rather similar to the Sun[8] located only 12.12 parsecs (39.5 ly) away.[9] Another solar analog in Serpens is the primary of Psi Serpentis, a binary star[10] located slightly further away at approximately 14.64 parsecs (47.7 ly).[11]

Beta, Gamma, and Iota Serpentis form a distinctive triangular shape marking the head of the snake, with Kappa Serpentis being roughly midway between Gamma and Iota. The brighest of the four with an apparent magnitude of 3.67, Beta Serpentis is a white main-sequence star roughly 155.0 parsecs (506 ly) distant.[12] It is likely that a nearby star of magnitude 9.95[13] is physically associated with Beta, although it is not certain.[14] The Mira variable R Serpentis, located between Beta and Gamma, is visible to the naked eye at its maximum brightness of 5.16, but typical of Mira variables, it can fade to below magnitude 14.[15] Gamma Serpentis itself is an F-type subgiant located only 11.25 parsecs (36.7 ly) distant and thus is quite bright, being of magnitude 3.84.[16] The star is known to show solar-like oscillations[17]

Delta Serpentis, forming part of the body of the snake between the heart and the head, is a multiple star system[18] located 69.93 parsecs (228.1 ly) light-years from Earth. Consisting of four stars, the system has a total apparent magnitude of 3.79 as viewed from Earth,[19] although two of the stars, with a combined apparent magntitude of 3.80, provide nearly all the light that reaches Earth.[20] The primary, a white subgiant, is a Delta Scuti variable with an average apparent magnitude of 4.23.[21] Located very near Delta, both in the night sky and likely in actual space at an estimated distance of 70.87 parsecs (231.1 ly),[22] is the barium star 16 Serpentis.[23] Another notable variable star visible to the naked eye is Chi Serpentis, an Alpha2 Canum Venaticorum variable located midway between Delta and Beta which varies from its median brightness of 5.33 by 0.03 magnitudes over a period of approximately 1.5 days.[24]

The two stars in Serpens Caput that form part of the Snake's body below the heart are Epsilon and Mu Serpentis, both third-magnitude A-type main-sequence stars.[25][26] Both have a peculiarity: Epsilon is an Am star,[27] while Mu is a binary.[28] Located slightly northwest of Mu is 36 Serpentis, another A-type main-sequence star. This star also has a peculiarity; it is a binary with the primary component being a Lambda Boötis star, meaning that it has solar-like amounts of carbon, nitrogen, and oxygen, while containing very low amounts of iron peak elements.[29] 25 Serpentis, located a few degrees northeast of Mu Serpentis, is a spectroscopic binary[30] consisting of a hot B-type giant and an A-type main-sequence star. The primary is a slowly pulsating B star, which causes the system to vary by 0.03 magnitudes.[31]

Serpens Caput contains many RR Lyrae variables, although most are too faint to be seen without professional equipment. The brightest is VY Serpentis, only of 10th magnitude. Interestingly, this star's period has been increasing by approximately 1.2 seconds per century.[32] A variable star of a different kind is Tau4 Serpentis, a cool red giant that pulsates between magnitudes 5.89 and 7.07 in 87 days.[33] This star has been found to display an inverse P Cygni profile.[34]

Several stars in Serpens have been found to have planets. The brightest, Omega Serpentis, located between Epsilon and Mu, is an orange giant with a planet of approximately 1.7 Jupiter-masses.[35] NN Serpentis, an eclipsing post-common-envelope binary consisting of a white dwarf and a red dwarf,[36] is very likely to have two planets causing variations in the period of the eclipses.[37]

One of the most interesting stellar remnants in the night sky is PSR B1534+11, a system consisting of two neutron stars in orbit around each other. One of the neutron stars is a pulsar with a period of 37.9 milliseconds. Located approximately 1,051 parsecs (3,430 ly) distant, the system demonstrates one of the best examples of general relativity.[38] The X-ray emission from the system has been found to be present when the non-pulsar star intersects the equatorial pulsar wind of the pulsar, and the system's orbit has been found to vary slightly.[39]

Tail stars

The constellation Serpens (Cauda) as it can be seen by the naked eye.

The brightest star in the tail, Eta Serpentis, is similar to Alpha Serpentis' primary in that it is a red giant of spectral class K. This star, however, is known to exhibit solar-like oscillations over a period of approximately 2.16 hours.[40] Eta Serpentis was previously classified as a carbon star, which would have made it the brightest carbon star in the sky, although this classification was found to be erroneous.[41]

The other two stars in Serpens Cauda forming its asterism are Theta and Xi Serpentis. Xi, where the asterism crosses over to Mu Serpentis in the head, is a triple star system[7] located approximately 105.2 parsecs (343 ly) away.[42] Two of the stars, with a combined apparent magnitude of 3.54, form a spectroscopic binary, and thus cannot be resolved with modern equipment. The primary is a white giant with an excess of strontium.[42] Theta, forming the tip of the tail, is also a multiple system, consisting of two A-type main-sequence stars with a combined apparent magnitude of 4.10 separated by almost half an arcminute.[7]

Lying near the boundary with Ophiuchus are Zeta (23.55 parsecs (76.8 ly) distant), Nu (209.3 parsecs (683 ly) distant), and Omicron Serpentis (173.1 parsecs (565 ly) distant). All three are 4th-magnitude main-sequence stars, with Nu and Omicron being of spectral type A[43][44] and Zeta being of spectral type F.[45] Nu is a binary star[7] with a secondary component of magnitude 9.3,[46] while Omicron is a Delta Scuti variable with amplitude variations of 0.01 magnitudes.[47] In 1909, the symbiotic nova[48] RT Serpentis appeared near Omicron, although it only reached a maximum magnitude of 10.2.[49]

The star system 59 Serpentis, also known as d Serpentis, is a triple star system [50] consisting of a spectroscopic binary containing an A-type star and an orange giant[51] and an orange giant secondary.[52] The system shows irregular variations in brightness between magnitudes 5.17 and 5.2.[53] In 1970, the nova FH Serpentis appeared just slightly north of 59 Serpentis, reaching a maximum brightness of 4.5.[54] Also near 59 Serpentis in the Serpens Cloud are several Orion variables. MWC 297 is a Herbig Be star that in 1994 exhibited a large X-ray flare and increased in X-ray luminosity by five times before returning to the quiescent state.[55] The star also appears to possess a circumstellar disk.[56] Another Orion variable in the region is VV Serpentis, a Herbig Ae star that has been found to exhibit Delta Scuti pulsations.[57] VV Serpentis has also, like MWC 297, been found to have a dusty disk surrounding it,[58] and is also a UX Orionis star,[59] meaning that it shows irregular variations in its brightness.

The star HR 6958, also known as MV Serpentis, is an Alpha2 Canum Venaticorum variable that is faintly visible to the naked eye.[60] The star's metal abundance is incredibly high for most metals at the iron peak and heavier, and has also been found to contain excess silicon.[61]

As the Milky Way passes through it, Serpens Cauda contains many massive OB stars. Several of these are visible to the naked eye, such as NW Serpentis, an early Be star that has been found to be somewhat variable. The variability is interesting; according to one study, it could be one of the first discovered hybrids between Beta Cephei variables and slowly pulsating B stars.[62] Although not visible to the naked eye, HD 167971 (MY Serpentis) is a Beta Lyrae variable triple system consisting of three very hot O-type stars. A member of the cluster NGC 6604,[63] the two eclipsing stars are both blue giants, with one being of the very early spectral type O7.5III. The remaining star is either a blue giant or supergiant of a late O or early B spectral type.[64] Also an eclipsing[65] binary, the HD 166734 system consists of two O-type blue supergiants in orbit around each other.[66]

South of the Eagle Nebula on the border with Sagittarius is the eclipsing binary W Serpentis, whose primary is a white giant that is interacting with the secondary. The system has been found to contain an accretion disk, and was one of the first discovered Serpentids, which are eclipsing binaries containing exceptionally strong far-ultraviolet spectral lines.[67] It is suspected that such Serpentids are in an earlier evolutionary phase, and will evolve first into double periodic variables and then classical Algol variables.[68] Also near the Eagle Nebula is the eclipsing Wolf–Rayet binary CV Serpentis, consisting of a Wolf–Rayet star and a hot O-type subgiant. The system is surrounded by a ring-shaped nebula, likely formed during the Wolf–Rayet phase of the primary.[69] The eclipses of the system very erratic, and although there are two theories as to why, neither of them is completely consistent with current understanding of stars.[70]

Serpens Cauda contains a few X-ray sources. One of these, GX 17+2, is a low-mass X-ray binary consisting of a neutron star and, as in all low-mass X-ray binaries, a low-mass star. The system has been classified as a Sco-like Z source, meaning that its accretion is near the Eddington limit.[71] The system has also been found to approximately every 3 days brighten by around 3.5 K-band magnitudes, possibly due to the presence of a synchrotron jet.[72] Another low-mass X-ray binary, Serpens X-1, undergoes occasional X-ray bursts. One in particular lasted nearly four hours, possibly explained by the burning of carbon in "a heavy element ocean".[73]

Deep-sky objects

Head objects

As the Milky Way does not pass through this part of Serpens, a view to many galaxies beyond it is possible. However, a few structures of the Milky Way Galaxy are present in Serpens Caput, such as Messier 5, a globular cluster located approximately 8° southwest of α Serpentis, right next to the star 5 Serpentis, a magnitude 5.05 star which was formerly thought to be variable but is now known not to be.[74] Although both designations contain a "5", this is purely coincidental. Messier 5 itself is located approximately 25000 ly distant[75] and, interestingly, contains two millisecond pulsars, one of which is in a binary.[76] The cluster has been used to test for magnetic dipole moments in neutrinos, which could shed light on some hypothetical particles such as the axion.[77]

Hoag's Object is a perfectly shaped ring galaxy located 600 million light-years from Earth (redshift 0.00425). The outer ring is largely composed of young blue stars but the core is made up of older yellow stars. The predominant theory regarding its formation is that the progenitor galaxy was a barred spiral galaxy whose arms had a velocity too great to keep its coherence and therefore detached.[78]

Arp 220 is another unusual galaxy in Serpens. The prototypical ultraluminous infrared galaxy, Arp 220 is located 250 million light-years from Earth (redshift 0.0181). It consists of two large spiral galaxies in the process of colliding with their nuclei orbiting at a distance of 1,200 light-years, causing extensive star formation throughout both components. It possesses a large cluster of more than a billion stars, partially covered by thick dust clouds near one of the galaxies' core.[78]

Seyfert's Sextet is a group of six galaxies, four of which are interacting gravitationally and two of which simply appear to be a part of the group despite their greater distance. The gravitationally bound cluster lies at a distance of 190 million light-years from Earth (redshift 0.0145) and is approximately 100,000 light-years across, making Seyfert's Sextet one of the densest galaxy clusters known. Astronomers predict that the four interacting galaxies will eventually merge to form a large elliptical galaxy.[78]

Tail objects

Part of the Milky Way passes through the tail, and thus Serpens Cauda is rich in deep-sky objects witin our own galaxy. The Eagle Nebula and its associated star cluster, Messier 16 lie 7,000 light-years from Earth in the direction of the galactic center. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. The stars being born in the Eagle Nebula, added to those with an approximate age of 5 million years have an average temperature of 45,000 kelvins and produce prodigious amounts of radiation that will eventually destroy the dust pillars.[78] Despite its fame, the Eagle Nebula is fairly dim, with an integrated magnitude of approximately 6.0. The star-forming regions in the nebula are often evaporating gaseous globules; unlike Bok globules they only hold one protostar.[79]

MWC 922 is a star surrounded by a planetary nebula. Dubbed the Red Square Nebula due to its similarities to the Red Rectangle Nebula, the planetary nebula appears to be a nearly perfect square with a dark band around the equatorial regions. The nebula contains concentric rings, which are similar to those seen in the supernova SN 1987A.[80] MWC 922 itself is an FS Canis Majoris variable,[81] meaning that it is a Be star containing exceptionally bright hydrogen emission lines as well as select forbidden lines, likely due to the presence of a close binary.[82]

The Serpens South star cluster was uncovered by NASA's Spitzer Space Telescope in the southern portion of the Serpens cloud. The discovery was possible due to the infrared observation capabilities of the SST because at visible wavelengths the stars are completely obscured by interstellar dust in the Serpens cloud.

Meteor showers

There are two daytime meteor showers that radiate from Serpens, the Omega Serpentids and the Sigma Serpentids. Both showers peak between December 18 and December 25.[83]

References

  1. ^ a b c d Ridpath, Ian. "Serpens". Star Tales. self-published. Retrieved 15 May 2014.
  2. ^ Gavin White, Babylonian Star-Lore (2007), p. 180.
  3. ^ a b Ridpath, Ian. "Constellations: Andromeda–Indus". Star Tales. self-published. Retrieved 1 April 2014.
  4. ^ "Caelum, Constellation Boundary". The Constellations. International Astronomical Union. Retrieved 20 April 2014.
  5. ^ Russell, H. N. (1922). "The New International Symbols for the Constellations". Popular Astronomy. 30: 469–71. Bibcode:1922PA.....30..469R.
  6. ^ "* Alpha Serpentis – Star in double system". SIMBAD. Retrieved 18 April 2014.
  7. ^ a b c d Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1111/j.1365-2966.2008.13596.x, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1111/j.1365-2966.2008.13596.x instead.
  8. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/201118751, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361/201118751 instead.
  9. ^ "* Lambda Serpentis – Star". SIMBAD. Retrieved 20 May 2014.
  10. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0004-6256/138/1/312, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0004-6256/138/1/312 instead.
  11. ^ "* Psi Serpentis – Double or multiple star". SIMBAD. Retrieved 21 June 2014.
  12. ^ "* Beta Serpentis – Star in double system". SIMBAD. Retrieved 12 May 2014.
  13. ^ "* Beta Serpentis B – Star in double system". SIMBAD. Retrieved 12 May 2014.
  14. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0067-0049/192/1/2, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0067-0049/192/1/2 instead.
  15. ^ VSX (4 January 2010). "R Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 22 May 2014.
  16. ^ "* Gamma Serpentis – Variable star". SIMBAD. Retrieved 22 May 2014.
  17. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/521575, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1086/521575 instead.
  18. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/201219774, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361/201219774 instead.
  19. ^ "* Delta Serpentis – Double or multiple star". SIMBAD. Retrieved 18 May 2014.
  20. ^ "* Delta Serpentis B – Star in double system". SIMBAD. Retrieved 18 May 2014.
  21. ^ VSX (4 January 2010). "Delta Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 18 May 2014.
  22. ^ "* 16 Serpentis – Star". SIMBAD. Retrieved 24 May 2014.
  23. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/164821, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1086/164821 instead.
  24. ^ VSX (4 January 2010). "Chi Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 26 May 2014.
  25. ^ "* Epsilon Serpentis – Star". SIMBAD. Retrieved 26 May 2014.
  26. ^ "* Mu Serpentis – Star". SIMBAD. Retrieved 26 May 2014.
  27. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1046/j.1365-8711.1998.01859.x, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1046/j.1365-8711.1998.01859.x instead.
  28. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1016/j.newast.2009.09.006, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1016/j.newast.2009.09.006 instead.
  29. ^ Nikolov, G.; Atanasova, E.; Iliev, I. K.; Paunzen, E.; Barzova, I. S. (April 2008). "Spectroscopic orbit determination of two metal-weak dwarf stars: HD64491 and HD141851". Contributions of the Astronomical Observatory Skalnaté Pleso. 38 (2): 433–434. Bibcode:2008CoSka..38..433N.
  30. ^ Petrie, R. M.; Phibbs, E. (1950). "Redetermination of the spectrographic orbits of iot Peg and 25 Ser". Publications of the Dominion Astrophysical Observatory Victoria. 8: 225. Bibcode:1950PDAO....8..225P.
  31. ^ VSX; Otero, S. A (10 February 2012). "PT Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 28 May 2014.
  32. ^ Wunder, E. (October 1991). "Period Changes of Bright RR Lyrae Stars SU Dra and VY Ser". Information Bulletin on Variable Stars. 3669 (1): IBVS Homepage. Bibcode:1991IBVS.3669....1W.
  33. ^ VSX; Otero, S. A (28 June 2012). "Tau4 Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 24 June 2014.
  34. ^ Kolotilov, E. A.; Russev, R. M. (January 1980). "Inverse P Cyg Profile of Halpha in the Spectrum of the Red Giant HD 139216 = tau4 Ser". Information Bulletin on Variable Stars. 1730: 1. Bibcode:1980IBVS.1730....1K.
  35. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1093/pasj/65.4.85, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1093/pasj/65.4.85 instead.
  36. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1111/j.1365-2966.2009.16072.x, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1111/j.1365-2966.2009.16072.x instead.
  37. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1093/mnras/stt1903, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1093/mnras/stt1903 instead.
  38. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0004-637X/787/1/82, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0004-637X/787/1/82 instead.
  39. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0004-637X/741/1/65, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0004-637X/741/1/65 instead.
  40. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/200912777, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361/200912777 instead.
  41. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1134/1.1398919, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1134/1.1398919 instead.
  42. ^ a b "Xi Serpentis – Spectroscopic binary". SIMBAD. Retrieved 21 June 2014.
  43. ^ "Nu Serpentis – Star in double system". SIMBAD. Retrieved 20 June 2014.
  44. ^ "Omicron Serpentis – Variable Star of delta Sct type". SIMBAD. Retrieved 20 June 2014.
  45. ^ "Zeta Serpentis – Star". SIMBAD. Retrieved 20 June 2014.
  46. ^ "BD-12 4724 – Star in double system". SIMBAD. Retrieved 20 June 2014.
  47. ^ VSX (4 January 2010). "Omicron Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 20 June 2014.
  48. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1007/BF02044949, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1007/BF02044949 instead.
  49. ^ VSX; Osborne, W. (1 April 2014). "RT Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 28 May 2014.
  50. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/144577, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1086/144577 instead.
  51. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0067-0049/180/1/117, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0067-0049/180/1/117 instead.
  52. ^ "HD 169986 – Star in double system". SIMBAD. Retrieved 25 May 2014.
  53. ^ VSX (4 January 2010). "d Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 25 May 2014.
  54. ^ VSX (28 April 2010). "FH Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 23 June 2014.
  55. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/308607, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1086/308607 instead.
  56. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361:200809654, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361:200809654 instead.
  57. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361:20065728, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361:20065728 instead.
  58. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/587935, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1086/587935 instead.
  59. ^ VSX; Otero, S. A. (23 November 2011). "VV Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 28 May 2014.
  60. ^ VSX (4 January 2010). "MV Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 25 May 2014.
  61. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361:20000438, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361:20000438 instead.
  62. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361:20077414, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361:20077414 instead.
  63. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361:20052810, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361:20052810 instead.
  64. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1093/mnras/stt1616, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1093/mnras/stt1616 instead.
  65. ^ VSX (4 January 2010). "V411 Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 25 May 2014.
  66. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/157971, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1086/157971 instead.
  67. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/175883, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1086/175883 instead.
  68. ^ Mennickent, R. E.; Kolaczkowski, Z. (2009). "Interacting Binary Star Environments and the W Ser - DPV - Algol Connection". arXiv:0904.1539 [astro-ph.SR].
  69. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/340725, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1086/340725 instead.
  70. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1111/j.1365-2966.2012.21736.x, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1111/j.1365-2966.2012.21736.x instead.
  71. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0004-637X/756/1/34, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0004-637X/756/1/34 instead.
  72. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0004-637X/701/2/L110, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0004-637X/701/2/L110 instead.
  73. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361:20011591, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361:20011591 instead.
  74. ^ VSX; Otero, S. A. (4 January 2010). "MQ Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 22 May 2014.
  75. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0004-6256/139/2/476, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0004-6256/139/2/476 instead.
  76. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/587832, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1086/587832 instead.
  77. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/201322004, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361/201322004 instead.
  78. ^ a b c d Wilkins, Jamie; Dunn, Robert (2006). 300 Astronomical Objects: A Visual Reference to the Universe (1st ed.). Buffalo, New York: Firefly Books. ISBN 978-1-55407-175-3.
  79. ^ Levy 2005, pp. 112–113.
  80. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1126/science.1135950, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1126/science.1135950 instead.
  81. ^ Plummer, A.; Otero, S. A. (27 March 2013). "MWC 922". AAVSO Website. American Association of Variable Star Observers. Retrieved 11 May 2014.
  82. ^ Otero, S. A.; Watson, C.; Wils, P. "Variable Star Type Designations in the VSX". AAVSO Website. American Association of Variable Star Observers. Retrieved 11 May 2014.
  83. ^ Jenniskens, Peter (September 2012). "Mapping Meteoroid Orbits: New Meteor Showers Discovered". Sky & Telescope: 24.
  • Levy, David H. (2005). Deep Sky Objects. Prometheus Books. ISBN 1-59102-361-0. {{cite book}}: Invalid |ref=harv (help)
  • Ian Ridpath and Wil Tirion (2007). Stars and Planets Guide, Collins, London. ISBN 978-0-00-725120-9. Princeton University Press, Princeton. ISBN 978-0-691-13556-4.
Wikimedia Commons has media related to Serpens.
Retrieved from "https://en.wikipedia.org/w/index.php?title=Serpens&oldid=621851496"