Editing Apus (section)

===Stars===
{{See also|List of stars in Apus}}
Lacaille gave twelve stars [[Bayer designation]]s, labelling them Alpha through to Kappa, including two stars next to each other as Delta and another two stars near each other as Kappa.<ref name=wagman/> Within the constellation's borders, there are 39 stars brighter than or equal to [[apparent magnitude]]&nbsp;6.5.{{efn|1=Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban-rural transition night skies.<ref>{{cite web|url=http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y|title=The Bortle Dark-Sky Scale|last=Bortle|first=John E.|date=February 2001|work=[[Sky & Telescope]]|access-date=26 August 2015|archive-date=31 March 2014|archive-url=https://web.archive.org/web/20140331202746/http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y|url-status=dead}}</ref>}}<ref name=tirionconst/> [[Beta Apodis|Beta]], [[Gamma Apodis|Gamma]] and [[Delta Apodis]] form a narrow triangle, with [[Alpha Apodis]] lying to the east.<ref>{{cite book |last=Thompson |first=Mark |title=A Down to Earth Guide to the Cosmos |publisher=Random House |date=2013 | location=New York, New York |isbn=978-1-4481-2691-0 |url=https://books.google.com/books?id=SOfRFJBy-igC&pg=PT161}}</ref> The five brightest stars are all red-tinged, which is unusual among constellations.<ref name=arnold>{{cite book |author1=Arnold, H.J.P |author2=Doherty, Paul |author3=Moore, Patrick |title=The Photographic Atlas of the Stars |publisher=CRC Press |location=Boca Raton, Florida |date=1999 |page=144 |isbn=978-0-7503-0654-6 |url=https://books.google.com/books?id=YjcvJUfnWBAC&pg=PA144}}</ref>

Alpha Apodis is an [[giant star|orange giant]] of spectral type K3III located 430 ± 20 [[light-year]]s away from Earth,<ref name=dr2>{{cite DR2}}</ref> with an apparent magnitude of 3.8.<ref name=ridpath01>{{cite book |last = Ridpath |first = Ian |date = 2017 |title = Stars and Planets Guide |publisher = Princeton University Press |location=Princeton, New Jersey |isbn = 978-0-691-17788-5 |pages=78–79}}</ref> It spent much of its life as a [[B-type main-sequence star|blue-white (B-type) main sequence star]] before expanding, cooling and brightening as it used up its core hydrogen.<ref name=kaler>{{cite web | title=Alpha Aps | work=Stars | first=James B. | last=Kaler | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/alphaaps.html | date=6 April 2007 | access-date=30 March 2016}}</ref> It has swollen to 48 times the Sun's diameter,<ref name=aaa367_521>{{cite journal | last1=Pasinetti Fracassini | first1=L. E. | last2=Pastori | first2=L. | last3=Covino | first3=S. | last4=Pozzi | first4=A. | title=Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics | journal=Astronomy and Astrophysics | volume=367 | issue=2 | pages=521–524 | date=2001 | doi=10.1051/0004-6361:20000451 | bibcode=2001A&A...367..521P | arxiv=astro-ph/0012289| s2cid=425754 }}</ref> and shines with a [[luminosity]] approximately 928 times that of the Sun, with a surface temperature of 4312 [[Kelvin|K]].<ref name=Mcdonald>{{cite journal|author=McDonald, I.|author2=Zijlstra, A. A.|author3=Boyer, M. L.|date=2012|title=Fundamental Parameters and Infrared Excesses of Hipparcos Stars|journal=Monthly Notices of the Royal Astronomical Society|volume=427|issue=1|pages=343–57|bibcode=2012MNRAS.427..343M|arxiv = 1208.2037 |doi = 10.1111/j.1365-2966.2012.21873.x |doi-access=free |s2cid=118665352}}</ref> Beta Apodis is an orange giant 149 ± 2 light-years away,<ref name=dr2/> with a magnitude of 4.2.<ref name=ridpath01/> It is around 1.84 times as massive as the Sun, with a surface temperature of 4677 K.<ref>{{cite journal|author=Liu, Y. J.|author2=Zhao, G.|author3=Shi, J. R.|author4=Pietrzyński, G.|author5=Gieren, W.|date=2007|title=The abundances of nearby red clump giants|journal=Monthly Notices of the Royal Astronomical Society|volume=382|issue=2|pages=553–66|bibcode=2007MNRAS.382..553L |doi=10.1111/j.1365-2966.2007.11852.x|doi-access=free}}</ref> Gamma Apodis is a [[giant star|yellow giant]] of spectral type G8III located 150 ± 4 light-years away,<ref name=dr2/> with a magnitude of 3.87. It is approximately 63 times as luminous the Sun, with a surface temperature of 5279 K.<ref name=Mcdonald/> Delta Apodis is a [[double star]], the two components of which are 103 arcseconds apart and visible through binoculars.<ref>{{cite book |last1=Privett |first1=Grant |last2=Jones |first2=Kevin |title=The Constellation Observing Atlas |publisher=Springer Science & Business Media |location=New York, New York |date=2013 |page=13 |isbn=978-1-4614-7648-1 |url=https://books.google.com/books?id=uN69BAAAQBAJ&pg=PA13}}</ref> Delta<sup>1</sup> is a [[red giant]] star of spectral type M4III located 630 ± 30 light-years away.<ref name=dr2/> It is a semiregular variable that varies from magnitude +4.66 to +4.87,<ref name=AAVSOdel1>{{cite web|url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=842 |title=Delta1 Apodis |author =Watson, Christopher |date=25 August 2009 |work=The International Variable Star Index|publisher=American Association of Variable Star Observers|access-date=30 March 2016}}</ref> with pulsations of multiple periods of 68.0, 94.9 and 101.7 days.<ref name=tabur>{{cite journal | title=Long-term photometry and periods for 261 nearby pulsating M giants | author=Tabur, V. | author2=Bedding, T.R. |author3=Kiss, L.L. | author4=Moon, T.T. | author5=Szeidl, B. | author6=Kjeldsen, H. |date=2009 |journal=Monthly Notices of the Royal Astronomical Society |volume= 400 | issue =4 |pages= 1945–61 |doi=10.1111/j.1365-2966.2009.15588.x | doi-access=free |arxiv = 0908.3228 |bibcode = 2009MNRAS.400.1945T | s2cid=15358380 }}</ref> Delta<sup>2</sup> is an [[orange giant]] star of spectral type K3III,<ref>{{cite journal|bibcode=1975mcts.book.....H|title=University of Michigan Catalogue of two-dimensional spectral types for the HD stars. Volume I. Declinations −90_ to −53_ƒ0|journal=University of Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars. Volume I. Declinations −90° to −53.0°|last1=Houk|first1=N.|last2=Cowley|first2=A. P.|year=1975}}</ref> located 550 ± 10 light-years away,<ref name=dr2/> with a magnitude of 5.3. The separate components can be resolved with the naked eye.<ref name=ridpath01/>

The fifth-brightest star is [[Zeta Apodis]] at magnitude 4.8,<ref name=arnold/> a star that has swollen and cooled to become an orange giant of spectral type K1III, with a surface temperature of 4649 K and a luminosity 133 times that of the Sun.<ref name=Mcdonald/> It is 300 ± 4 light-years distant.<ref name=dr2/> Near Zeta is [[Iota Apodis]], a [[binary star]] system 1,040 ± 60 light-years distant,<ref name=dr2/> that is composed of two blue-white main sequence stars that orbit each other every 59.32 years. Of spectral types B9V and B9.5 V, they are both over three times as massive as the Sun.<ref>{{cite journal | title=Dynamical and physical properties of 22 binaries discovered by W. S. Finsen|author1=Docobo, J.A. |author2=Andrade, M. |journal=Monthly Notices of the Royal Astronomical Society|volume =428 |issue =1| pages=321–39| year= 2013|doi=10.1093/mnras/sts045 | bibcode=2013MNRAS.428..321D|doi-access=free}}</ref>

[[Eta Apodis]] is a [[A-type main-sequence star|white main sequence star]] located 140.8 ± 0.9 light-years distant.<ref name=dr2/> Of apparent magnitude 4.89, it is 1.77 times as massive, 15.5 times as luminous as the Sun and has 2.13 times its radius. Aged 250 ± 200 million years old, this star is emitting an [[infrared excess|excess]] of 24&nbsp;μm infrared radiation, which may be caused by a [[debris disk]] of dust orbiting at a distance of more than 31 [[astronomical unit]]s from it.<ref name="apj698">{{cite journal | last1=Plavchan | first1=Peter | last2=Werner | first2=M.W. | last3=Chen | first3=C.H. | last4=Stapelfeldt | first4=K.R. | last5=Su | first5=K.Y.L. | last6=Stauffer | first6=J.R. | last7=Song | first7=I. | title=New Debris Disks Around Young, Low-Mass Stars Discovered with the Spitzer Space Telescope | journal=The Astrophysical Journal | volume=698 | issue=2 | pages=1068–94 |date=2009 | doi=10.1088/0004-637X/698/2/1068 | bibcode=2009ApJ...698.1068P |arxiv = 0904.0819 | s2cid=51417657 }}</ref><!-- cites prev 2 sentences -->

[[Theta Apodis]] is a cool red giant of spectral type M7 III located 350 ± 30 light-years distant.<ref name=dr2/> It shines with a luminosity approximately 3879 times that of the Sun and has a surface temperature of 3151 K.<ref name=Mcdonald/> A semiregular variable, it varies by 0.56 magnitudes with a period of 119 days<ref name=mnras355_2_601>{{cite journal| last1=Yeşilyaprak | first1=C. | last2=Aslan | first2=Z. | title=Period-luminosity relation for M-type semiregular variables from Hipparcos parallaxes | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=355 | issue=2 | pages=601–07 |date=2004 | doi=10.1111/j.1365-2966.2004.08344.x | bibcode=2004MNRAS.355..601Y| doi-access=free }}</ref>—or approximately 4 months.<ref name=ridpath01/> It is losing mass at the rate of {{nowrap|1.1 × 10<sup>−7</sup>}} times the mass of the Sun per year through its [[stellar wind]]. Dusty material ejected from this star is interacting with the surrounding [[interstellar medium]], forming a [[bow shock]] as the star moves through the galaxy.<ref name=aaa537_A35>{{cite journal | last1=Cox | first1=N.L.J. | last2=Kerschbaum | first2=F. | last3=van Marle | first3=A.-J. | last4=Decin | first4=L. | last5=Ladjal | first5=D. | last6=Mayer | first6=A. | last7=Groenewegen | first7=M. A. T. | last8=van Eck | first8=S. | last9=Royer | first9=P. | last10=Ottensamer | first10=R. | last11=Ueta | first11=T. | last12=Jorissen | first12=A. | last13=Mecina | first13=M. | last14=Meliani | first14=Z. | last15=Luntzer | first15=A. | last16=Blommaert | first16=J.A.D.L. | last17=Posch | first17=Th. | last18=Vandenbussche, B. | last19=Waelkens, C. | title=A far-infrared survey of bow shocks and detached shells around AGB stars and red supergiants | journal=Astronomy & Astrophysics | volume=537 | page=A35 |date=2012 | doi=10.1051/0004-6361/201117910 | bibcode=2012A&A...537A..35C |arxiv = 1110.5486 | s2cid=56041336 }} See table 1, IRAS 14003-7633.</ref> [[NO Apodis]] is a red giant of spectral type M3III that varies between magnitudes 5.71 and 5.95.<ref name=AAVSONO>{{cite web|url=http://www.aavso.org/vsx/index.php?view=detail.top&oid=815 |title=NO Apodis |author =Watson, Christopher |date=25 August 2009 |work=The International Variable Star Index|publisher=American Association of Variable Star Observers|access-date=31 March 2015}}</ref> Located 780 ± 20 light-years distant, it shines with a luminosity estimated at 2059 times that of the Sun and has a surface temperature of 3568 K.<ref name=Mcdonald/> [[S Apodis]] is a rare [[R Coronae Borealis variable]], an extremely hydrogen-deficient supergiant thought to have arisen as the result of the merger of two white dwarfs; fewer than 100 have been discovered as of 2012. It has a baseline magnitude of 9.7.<ref name=tisserand>{{cite journal |author1=Tisserand|author2=Clayton|author3=Welch|author4=Pilecki|author5=Wyrzykowski|author6=Kilkenny|title=The Ongoing Pursuit of R Coronae Borealis Stars: ASAS-3 Survey Strikes Again |date=2012 |bibcode=2013A&A...551A..77T |journal =Astronomy & Astrophysics |volume = 551 | id = A77 |pages= 22|arxiv = 1211.2475 |doi = 10.1051/0004-6361/201220713 |s2cid=59060842}}</ref> [[R Apodis]] is a star that was given a [[variable star designation]], yet has turned out not to be variable. Of magnitude 5.3,<ref name=arnold/> it is another orange giant.

Two star systems have had [[exoplanet]]s discovered by [[doppler spectroscopy]], and the substellar companion of a third star system—the sunlike star [[HD 131664]]—has since been found to be a [[brown dwarf]] with a calculated mass of the companion to 23 times that of Jupiter (minimum of 18 and maximum of 49 Jovian masses).<ref name="ReffertQuirrenbach">{{cite journal|author1=Reffert, S.|author2=Quirrenbach, A.|title=Mass constraints on substellar companion candidates from the re-reduced Hipparcos intermediate astrometric data: nine confirmed planets and two confirmed brown dwarfs|date=2011|journal=Astronomy & Astrophysics|volume=527|pages=A140 |doi=10.1051/0004-6361/201015861|bibcode=2011A&A...527A.140R|arxiv=1101.2227|s2cid=54986291}}</ref> [[HD 134606]] is a yellow sunlike star of spectral type G6IV that has begun expanding and cooling off the [[main sequence]].<ref name="Gray">{{cite journal | last1=Gray | first1=R.O.| last2=Corbally | first2=C.J.| last3=Garrison | first3=R.F.| last4=McFadden | first4=M.T. | last5=Bubar | first5=E.J. | last6=McGahee | first6=C.E.| last7=O'Donoghue | first7=A.A.| last8=Knox | first8=E.R.| title=Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample | journal=[[The Astronomical Journal]] | volume=132 | issue=1 | pages=161–170 | date=July 2006 | doi=10.1086/504637 | bibcode=2006AJ....132..161G | arxiv=astro-ph/0603770| s2cid=119476992}}</ref> Three planets orbit it with periods of 12, 59.5 and 459 days, successively larger as they are further away from the star.<ref>{{cite journal | title=Tests of in situ Formation Scenarios for Compact Multiplanet Systems |author=Schlaufman, Kevin C. | journal=The Astrophysical Journal |volume = 790|issue =2| id= 91 |pages= 11 |year=2014| doi=10.1088/0004-637X/790/2/91 |bibcode=2014ApJ...790...91S|arxiv=1402.7075|s2cid=8130257 }}</ref> [[HD 137388]] is another star—of spectral type K2IV—that is cooler than the Sun and has begun cooling off the main sequence.<ref name="Gray"/> Around 47% as luminous and 88% as massive as the Sun, with 85% of its diameter, it is thought to be around 7.4 ± 3.9 billion years old.<ref name=" Bonfanti 2015">{{cite journal|author1=Bonfanti, A. |author2=Ortolani, S. |author3=Piotto, G. |author4=Nascimbeni, V. |date=2015|title=Revising the ages of planet-hosting stars|journal=Astronomy & Astrophysics|volume=575|issue=A18|pages=17|doi=10.1051/0004-6361/201424951 |bibcode=2015A&A...575A..18B|arxiv = 1411.4302 |s2cid=54555839 }}</ref> It has a planet that is 79 times as massive as the Earth and orbits its sun every 330 days at an average distance of 0.89 astronomical units (AU).<ref name=HARPSXXX>{{cite journal |title=The HARPS Search for Southern Extra-solar Planets. XXX. Planetary Systems around Stars with Solar-like Magnetic Cycles and Short-term Activity Variation |author1=Dumusque, X. |author2=Lovis, C. |author3=Ségransan, D. |author4=Mayor, M. |author5=Udry, S. |author6=Benz, W. |author7=Bouchy, F. |author8=Lo Curto, G. |author9=Mordasini, C. |author10=Pepe, F. |author11=Queloz, D. |author12=Santos, N. C. |author13=Naef, D. |journal=Astronomy & Astrophysics |volume=535 |pages=A55–A66 |doi=10.1051/0004-6361/201117148 |url=http://cds.aanda.org/articles/aa/full_html/2011/11/aa17148-11/aa17148-11.html |arxiv=1107.1748 |bibcode=2011A&A...535A..55D |year=2011 |s2cid=119192207 |access-date=2016-05-29 |archive-url=https://web.archive.org/web/20150529071847/http://cds.aanda.org/articles/aa/full_html/2011/11/aa17148-11/aa17148-11.html |archive-date=2015-05-29 |url-status=dead }}</ref>