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Delphinus
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===Stars=== {{See also|List of stars in Delphinus}} Delphinus has two stars above fourth [[apparent magnitude|(apparent) magnitude]]; its brightest star is of magnitude 3.6. The main [[asterism (astronomy)|asterism]] in Delphinus is Job's Coffin, nearly a 45°-apex [[lozenge (shape)|lozenge]] or diamond of the four brightest stars: Alpha, Beta, Gamma, and Delta Delphini. Delphinus is in a rich Milky Way star field. Alpha and Beta Delphini have 19th-century names Sualocin and Rotanev, read backwards: Nicolaus Venator, the Latinized name of a [[Palermo Astronomical Observatory|Palermo Observatory]] director, [[Niccolò Cacciatore]] (d. 1841).{{sfn|Ridpath|Tirion|2017|pp=140-141}} [[Alpha Delphini]] is a blue-white hued [[main sequence]] star of magnitude 3.8,<ref name=oja>{{cite journal|bibcode=1991A&AS...89..415O|title=UBV photometry of stars whose positions are accurately known. VI|journal=Astronomy and Astrophysics Supplement Series|volume=89|pages=415|last1=Oja|first1=T.|year=1991}}</ref> 241 light-years from Earth. It is a spectroscopic binary.<ref name=malkov>{{cite journal|bibcode=2012A&A...546A..69M|title=Dynamical masses of a selected sample of orbital binaries|journal=Astronomy & Astrophysics|volume=546|pages=A69|last1=Malkov|first1=O. Yu.|last2=Tamazian|first2=V. S.|last3=Docobo|first3=J. A.|last4=Chulkov|first4=D. A.|year=2012|doi=10.1051/0004-6361/201219774|doi-access=free}}</ref> It is officially named Sualocin.<ref name=Kunitzsch>{{cite book |last1=Kunitzsch |first1=Paul |last2=Smart |first2=Tim |date = 2006 |edition = 2nd rev. |title = A Dictionary of Modern Star Names: A Short Guide to 254 Star Names and Their Derivations |publisher = Sky Pub |location = Cambridge, Massachusetts |isbn = 978-1-931559-44-7 }}</ref><ref name=Sualocin>{{cite web | url=https://www.iau.org/public/themes/naming_stars/ | title=Naming Stars |publisher=IAU.org |accessdate=16 December 2017}}</ref> The star has an absolute magnitude of -0.4.<ref name=mv>{{cite journal|bibcode=1998A&A...330..619J|title=The absolute magnitude of the early type MK standards from HIPPARCOS parallaxes|journal=Astronomy and Astrophysics|volume=330|pages=619|last1=Jaschek|first1=C.|last2=Gomez|first2=A. E.|year=1998}}</ref> [[Beta Delphini]] is officially called Rotanev.<ref name=Kunitzsch/> It was found to be a binary star in 1873.<ref name=burnham1978>{{citation | first1=Robert | last1=Burnham | title=Burnham's celestial handbook: an observer's guide to the universe beyond the Solar System | volume=2 | series=Dover Books on Astronomy | edition=2nd | publisher=[[Courier Dover Publications]] | year=1978 | isbn=0-486-23568-8 | page=820 | url=https://books.google.com/books?id=wB9uZ9lH5bgC&pg=PA820 }}</ref> The gap between its close [[binary star|binary]] stars is visible from large amateur telescopes. To the unaided eye, it appears to be a white star of magnitude 3.6.<ref name=aj138_5_1354>{{citation | display-authors=1 | last1=Davidson | first1=James W. Jr. | last2=Baptista | first2=Brian J. | last3=Horch | first3=Elliott P. | last4=Franz | first4=Otto | last5=van Altena | first5=William F. | title=A Photometric Analysis of Seventeen Binary Stars Using Speckle Imaging | journal=The Astronomical Journal | volume=138 | issue=5 | pages=1354–1364 |date=November 2009 | doi=10.1088/0004-6256/138/5/1354 | bibcode=2009AJ....138.1354D | s2cid=122194357 | doi-access=free }}</ref><ref name=burnham1978 /> It has a period of 27 years and is 97 light-years from Earth. [[Gamma Delphini]] is a celebrated binary star among amateur astronomers. The primary is orange-gold of magnitude 4.3; the secondary is a light yellow star of magnitude 5.1. The pair forms a true binary with an estimated orbital period of over 3,000 years. 125 light-years away, the two components are visible in a small amateur telescope.{{sfn|Ridpath|Tirion|2017|pp=140-141}} The secondary, also described as green, is 10 arcseconds from the primary. [[Struve 2725]], called the "Ghost Double", is a pair that appears similar but dimmer. Its components of magnitudes 7.6 and 8.4 are separated by 6 arcseconds and are 15 arcminutes from Gamma Delphini itself.<ref name="S&T"/> An unconfirmed exoplanet with a minimum mass of 0.7 Jupiter masses may orbit one of the stars.<ref name=Irwin_et_al_1999>{{citation | title=A Program for the Analysis of Long-Period Binaries: The Case of γ Delphini | display-authors=1 | last1=Irwin | first1=A. W. | last2=Vandenberg | first2=D. A. | last3=Larson | first3=A. M. | work=Precise Stellar Radial Velocities. IAU Colloquium 170 | series=ASP Conference Series #185 | editor1-first=J. B. | editor1-last=Hearnshaw | editor2-first=C. D. | editor2-last=Scarfe | isbn=1-58381-011-0 | date=1999 | volume=185 | page=297 | bibcode=1999ASPC..185..297I }}</ref><ref name="Wittemeyer et al.">{{cite journal | display-authors=1 | last1=Wittemeyer | last2=Endl | first2=Michael | last3=Cochran | first3=William D. | last4=Hatzes | first4=Artie P. | last5=Walker | first5=G. A. H. | last6=Yang | first6=S. L. S. | last7=Paulson | first7=Diane B. | title=Detection Limits from the McDonald Observatory Planet Search Program | journal=[[The Astronomical Journal]] | volume=132 | issue=1 | pages=177–188 | date=2006 | bibcode=2006AJ....132..177W | arxiv=astro-ph/0604171 | doi=10.1086/504942 | s2cid=16755455 }}</ref> [[Delta Delphini]] is a type [[A-type main sequence star|A-type star]]<ref name=gray2001>{{citation | last1=Gray | first1=R. O. | last2=Napier | first2=M. G. | last3=Winkler | first3=L. I. | title=The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars | journal=The Astronomical Journal | volume=121 | issue=4 | pages=2148–2158 | date=April 2001 | doi=10.1086/319956 | bibcode=2001AJ....121.2148G | postscript=. | doi-access=free}}</ref> of magnitude 4.43.<ref name=Chang2013>{{citation | title=Statistical Properties of Galactic δ Scuti Stars: Revisited | last1=Chang | first1=S.-W. | last2=Protopapas | first2=P. | last3=Kim | first3=D.-W. | last4=Byun | first4=Y.-I. | journal=The Astronomical Journal | display-authors=1 | volume=145 | issue=5 | date=2013 | bibcode=2013AJ....145..132C | doi=10.1088/0004-6256/145/5/132 | arxiv=1303.1031 | postscript=. | page=132| s2cid=118900730 }}</ref> It is a spectroscopic binary, and both stars are [[Delta Scuti variable]]s.<ref name=Liakos2017>{{citation |postscript=. | title=Catalogue and properties of δ Scuti stars in binaries | last1=Liakos | first1=Alexios | last2=Niarchos | first2=Panagiotis | journal=Monthly Notices of the Royal Astronomical Society | volume=465 | issue=1 | pages=1181–1200 | date=February 2017 | doi=10.1093/mnras/stw2756 | doi-access=free | bibcode=2017MNRAS.465.1181L |arxiv = 1611.00200 }}</ref> [[Epsilon Delphini]], Deneb Dulfim ([[Arab astrology|lit.]] "tail [of the] Dolphin"), or Aldulfin, is a star of [[stellar classification|stellar class]] B6 III.<ref name=Lesh1968>{{citation | last=Lesh | first=Janet Rountree | postscript=. | title=The Kinematics of the Gould Belt: an Expanding Group? | journal=Astrophysical Journal Supplement | volume=17 | page=371 | date=December 1968 | doi=10.1086/190179 | bibcode=1968ApJS...17..371L | doi-access=free }}</ref> Its magnitude is variable at around 4.03.<ref>{{citation | display-authors=1 | last1=Samus | first1=N. N. | last2=Kazarovets | first2=E.V. | last3=Durlevich | first3=O.V. | last4=Kireeva | first4=N.N. | last5=Pastukhova | first5=E.N. | title=General Catalogue of Variable Stars | postscript=. | version=GCVS 5.1 | journal=Astronomy Reports | date=January 2017 | volume=61 | issue=1 | pages=80–88 | bibcode=2017ARep...61...80S | doi=10.1134/S1063772917010085 | s2cid=125853869 }}</ref><ref name=Crawford1971>{{citation | display-authors=1 | last1=Crawford | first1=D. L. | last2=Barnes | first2=J. V. | last3=Golson | first3=J. C. | title=Four-color, H-beta, and UBV photometry for bright B-type stars in the northern hemisphere | journal=The Astronomical Journal | year=1971 | pages=1058 | volume=76 | postscript=. | bibcode=1971AJ.....76.1058C | doi=10.1086/111220 }}</ref> [[Zeta Delphini]], an A3Va<ref name=Zeta /> main-sequence star of magnitude 4.6, was in 2014 discovered to have a [[brown dwarf]] orbiting around it. Zeta Delphini B has a mass of 50±15 {{jupiter mass}}.<ref name=Zeta>{{cite journal |last1=De Rosa |first1=R. J. |last2=Patience |first2=J. |last3=Ward-Duong |first3=K. |last4=Vigan |first4=A. |last5=Marois |first5=C. |last6=Song |first6=I. |last7=Macintosh |first7=B. |last8=Graham |first8=J. R. |last9=Doyon |first9=R. |last10=Bessell |first10=M. S. |last11=Lai |first11=O. |last12=McCarthy |first12=D. W. |last13=Kulesa |first13=C. |title=The VAST Survey - IV. A wide brown dwarf companion to the A3V star ζ Delphini |journal=Monthly Notices of the Royal Astronomical Society |date=December 2014 |volume=445 |issue=4 |page=3694 |doi=10.1093/mnras/stu2018 |arxiv=1410.0005 |bibcode=2014MNRAS.445.3694D |language=en |issn=0035-8711|doi-access=free }}</ref> [[Image:Aquila.fade-in.animation.webm|thumb|upright=1.2|right|Animation fading-in of [[Aquila (constellation)|Aquila]], Delphinus, [[Sagitta]], and the summer [[Milky Way]] as seen in [[Westhavelland Nature Park|Dark-sky preserve Westhavelland]]]] [[Rho Aquilae]] at magnitude 4.94<ref name=scfs /> is at about 150 light-years away.<ref name=scfs>{{citation | display-authors=1 | title=Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions | last1=Wielen | first1=R. | last2=Schwan | first2=H. | last3=Dettbarn | first3=C. | last4=Lenhardt | first4=H. | last5=Jahreiß | first5=H. | last6=Jährling | first6=R. | journal=Veroeffentlichungen des Astronomischen Rechen-Instituts Heidelberg | publisher=Astronomisches Rechen-Institut Heidelberg | issue=35 | year=1999 | volume=35 | page=1 | bibcode=1999VeARI..35....1W | postscript=. }}</ref> Due to its [[proper motion]], it has been in the (round-figure parameter) bounds of the constellation since 1992.<ref>{{cite book|author=Patrick Moore|title=The Observer's Year: 366 Nights of the Universe|url=https://books.google.com/books?id=p87TBwAAQBAJ&pg=PA132|date=29 June 2013|publisher=Springer Science & Business Media|isbn=978-1-4471-3613-2|pages=132–}}</ref> It is an [[A-type main sequence star]] with a lower metallicity than the Sun.<ref name=starhorse>{{citation |postscript=. |last1=Anders |first1=F. |last2=Khalatyan |first2=A. |last3=Chiappini |first3=C. |last4=Queiroz |first4=A. B. |last5=Santiago |first5=B. X. |last6=Jordi |first6=C. |last7=Girardi |first7=L. |last8=Brown |first8=A. G. A. |last9=Matijevic |first9=G. |last10=Monari |first10=G. |last11=Cantat-Gaudin |first11=T. |last12=Weiler |first12=M. |last13=Khan |first13=S. |last14=Miglio |first14=A. |last15=Carrillo |first15=I. |last16=Romero-Gómez |first16=M. |last17=Minchev |first17=I. |last18=de Jong |first18=R. S. |last19=Antoja |first19=T. |last20=Ramos |first20=P. |last21=Steinmetz |first21=M. |last22=Enke |first22=H. |title=Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18 |journal=Astronomy and Astrophysics |date=1 August 2019 |volume=628 |pages=A94 |doi=10.1051/0004-6361/201935765 |arxiv=1904.11302 |bibcode=2019A&A...628A..94A |s2cid=131780028 |issn=0004-6361}}</ref> [[HR Delphini]] was a [[nova]] that brightened to magnitude 3.5 in December 1967.<ref name=isles67>{{cite journal | title = HR Delphini (Nova 1967) in 1967 - 71 | author =Isles, J. E.|journal =Journal of the British Astronomical Association | volume= 85|pages= 54–58| year=1974|bibcode =1974JBAA...85...54I}}</ref> It took an unusually long time for the nova to reach peak brightness which indicate that it barely satisfied the conditions for a thermonuclear runaway.<ref>{{cite journal |last1=Friedjung |first1=M |title=The unusual nature of nova HR Delphini 1967 |journal=Astronomy & Astrophysics |date=17 March 1992 |volume=262 |issue=262 |page=487 |bibcode=1992A&A...262..487F |url=https://ui.adsabs.harvard.edu/abs/1992A%26A...262..487F/abstract |access-date=19 July 2020}}</ref> Another nova by the name [[V339 Delphini]] was detected in 2013; it peaked at magnitude 4.3 and was the first nova observed to produce lithium.<ref>{{cite journal |last1=Tajitsu |first1=Akito |last2=Sadakane |first2=Kozo |last3=Naito |first3=Hiroyuki |last4=Arai |first4=Akira |last5=Aoki |first5=Wako |title=Explosive lithium production in the classical nova V339 Del (Nova Delphini 2013) |journal=Nature |date=18 February 2015 |volume=518 |issue=7539 |pages=381–384 |doi=10.1038/nature14161|pmid=25693569 |arxiv=1502.05598 |bibcode=2015Natur.518..381T |s2cid=205242345 }}</ref><ref>{{cite web |url=http://www.universetoday.com/104103/bright-new-nova-in-delphinus-you-can-see-it-tonight-with-binoculars |author=King, Bob |title=Bright New Nova In Delphinus — You can See it Tonight With Binoculars |work=Universe Today (initial designation PNV J20233073+2046041) |date=August 14, 2013 |access-date=August 15, 2013}}</ref><ref>{{cite web |url=http://remanzacco.blogspot.it/2013/08/possible-bright-nova-in-delphinus.html |title=Possible Bright Nova in Delphinus |publisher=Associazione Friulana di Astronomia e Meteorologia |last1=Guido |first1=Ernesto| first2=Nello |last2=Ruocco |first3=Nick |last3=Howes |date=August 15, 2013 |access-date=August 15, 2013}}</ref><ref>{{cite web |url=http://www.virtualtelescope.eu/2013/08/15/possible-nova-pnv-j202330732046041-in-delphinus/ |title=Nova Delphini 2013 (formerly PNV J20233073+2046041): images, spectra and maps |publisher=[[Gianluca Masi]] - [[Virtual Telescope Project]] |last1=Masi|first1=Gianluca|date=August 15, 2013 |access-date=August 15, 2013}}</ref> [[Musica (star)|Musica]], also known by its Flamsteed designation 18 Delphini, is one of the five stars with known planets located in Delphinus. It has a spectral type of G6 III.<ref>{{cite journal | title=The spectrophotometric parallaxes of 42 visual binaries | last=Opolski | first=A. | journal=Arkiv för Astronomi | volume=2 | pages=55 | year= 1957 | bibcode=1957ArA.....2...55O }}</ref> [[Arion (planet)|Arion]], the planet, is a very dense and massive planet with a mass at least 10.3 times greater than Jupiter.<ref>{{cite journal |last1=Sato |first1=Bun’ei |last2=Izumiura |first2=Hideyuki |last3=Toyota |first3=Eri |last4=Kambe |first4=Eiji |last5=Ikoma |first5=Masahiro |last6=Omiya |first6=Masashi |last7=Masuda |first7=Seiji |last8=Takeda |first8=Yoichi |last9=Murata |first9=Daisuke |last10=Itoh |first10=Yoichi |last11=Ando |first11=Hiroyasu |last12=Yoshida |first12=Michitoshi |last13=Kokubo |first13=Eiichiro |last14=Ida |first14=Shigeru |title=Planetary Companions around Three Intermediate-Mass G and K Giants: 18 Delphini, ξ Aquilae, and HD 81688 |journal=Publications of the Astronomical Society of Japan |date=25 June 2008 |volume=60 |issue=3 |pages=539–550 |doi=10.1093/pasj/60.3.539 |arxiv=0802.2590 |bibcode=2008PASJ...60..539S |url=https://academic.oup.com/pasj/article/60/3/539/1508408 |language=en |issn=0004-6264|doi-access=free }}</ref> Arion was part of the first [[NameExoWorlds]] contest where the public got the opportunity to suggest names for exoplanets and their host stars.<ref>{{cite web |title=International Astronomical Union {{!}} IAU |url=https://www.iau.org/news/pressreleases/detail/iau1514/ |website=www.iau.org |access-date=19 July 2020}}</ref>
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