29 Aquarii

{{short description|Binary star in the constellation Aquarius}}

{{Starbox begin

| name = 29 Aquarii

}}

{{Starbox image

| image = 250px

| caption = The light curve of 29 Aquarii, from Hipparcos data

}}

{{Starbox observe

| epoch = J2000

| ra = {{RA|22|02|26.24845}}

| dec = {{DEC|-16|57|53.3959}}

| appmag_v = 6.39

| constell = Aquarius

}}

{{Starbox character

| class = {{nowrap|A2 V + K0 III}}

| b-v = {{Val|0.447|0.022}}

| u-b =

| variable =

}}

{{Starbox astrometry

| radial_v = {{Val|+15.0|4.3}}

| prop_mo_ra = +5.292

| prop_mo_dec = +1.256

| parallax = 5.5489

| p_error = 0.1285

| parallax_footnote =

| absmag_v =

}}

{{Starbox orbit

| reference =

| period =

| period_unitless = 0.945 d

| eccentricity = 0.00

| periastron = {{Val|2436814.418|1.0|ul=JD|fmt=commas}}

| k1 = 97.9

}}

{{Starbox catalog

| names = {{odlist | BD=−17°6422 | HD=209278 | HIP=108797 | HR=8396 | SAO=164830 | WDS=J22024-1658 }}

}}

{{Starbox reference

|Simbad=29+Aqr

}}

{{Starbox end}}

29 Aquarii is a binary star system located around 590 light years away from the Sun in the equatorial constellation of Aquarius. 29 Aquarii is the Flamsteed designation; the system also bears the variable star designation DX Aquarii. It is a challenge to view with the naked eye, appearing as a dim star with a combined apparent visual magnitude of 6.39. The system is moving further from the Earth with a heliocentric radial velocity of about +15 km/s.

This is a spectroscopic binary system with a close circular orbit taking just 0.945 days to complete. Despite their proximity, this does not appear to be a contact binary system. The orbital plane of the two stars lies near the line of sight, so they form an Algol-type eclipsing binary. The first component of the system is an A-type main sequence star with a stellar classification of A2 V. Its companion is giant star with a classification of K0 III.

The variability of this system was first noticed in 1965 by W. Strohmeier of Remeis-Observatory in Bamberg, Germany. He later discovered that the variability was caused by a binary companion eclipsing the primary star.

References

{{reflist|refs=

{{cite web |last1=Molik |first1=Petr |title=Eclipsing binary DX Aqr |url=http://www.petrmolik.cz/shonpost.htm |website=Sun Hill Observatory |access-date=16 October 2021}}

{{cite DR2|6826564991861746688}}

{{citation

| title=XHIP: An extended hipparcos compilation

| last1=Anderson | first1=E. | last2=Francis | first2=Ch.

| journal=Astronomy Letters | postscript=.

| volume=38 | issue=5 | pages=331 | year=2012

| bibcode=2012AstL...38..331A | arxiv=1108.4971

| doi=10.1134/S1063773712050015 | s2cid=119257644 }}

{{citation

| title=Spectroscopic orbits of the eclipsing binaries DV and CX Aqr

| last1=Paffhausen | first1=W. | last2=Seggewiss | first2=W.

| journal=Astronomy and Astrophysics, Supplemental Series

| volume=24 | pages=29–34 | date=April 1976

| bibcode=1976A&AS...24...29P | postscript=. }}

{{citation | first=F. | last=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 | postscript=. |arxiv = 0708.1752 | s2cid=18759600 }}

{{citation | display-authors=1 | last1=Zasche | first1=P. | last2=Wolf | first2=M. | last3=Hartkopf | first3=W. I. | last4=Svoboda | first4=P. | last5=Uhlař | first5=R. | last6=Liakos | first6=A. | last7=Gazeas | first7=K. | title=A Catalog of Visual Double and Multiple Stars With Eclipsing Components | journal=The Astronomical Journal | volume=138 | issue=2 | pages=664–679 | doi=10.1088/0004-6256/138/2/664 | bibcode=2009AJ....138..664Z | postscript=. |arxiv = 0907.5172 |date=August 2009| s2cid=17089387 }}

{{cite journal | title=Bright Southern BV-Stars | url=https://konkoly.hu/pub/ibvs/0001/0081.txt | last1=Strohmeier | first1=W. | last2=Knigge | first2=R. | last3=Ott | first3=H. | display-authors=1 | journal=Information Bulletin on Variable Stars | volume=81 | pages=1 | date=1965 | bibcode=1965IBVS...81....1S }}

{{cite journal | title=BV 449 and BV 600, Two Bright EB-Stars | url=http://www.konkoly.hu/cgi-bin/IBVS?0164 | archive-url=https://archive.today/20130818213255/http://www.konkoly.hu/cgi-bin/IBVS?0164 | url-status=dead | archive-date=August 18, 2013 | last1=Strohmeier | first1=W. | journal=Information Bulletin on Variable Stars | volume=164 | pages=1 | date=1966 | bibcode=1966IBVS..164....1S }}

{{citation | title=BD-17 6422 -- Spectroscopic binary | work=SIMBAD Astronomical Object Database | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=BD-17+6422 | access-date=2012-07-16 | postscript=. }}

{{citation

| title=The 7.5 Magnitude Limit Sample of Bright Short-Period Binary Stars. I. How Many Contact Binaries Are There?

| last1=Rucinski | first1=Slavek M.

| journal=The Publications of the Astronomical Society of the Pacific

| volume=114 | issue=800 | pages=1124–1142 | date=October 2002

| doi=10.1086/342677 | arxiv=astro-ph/0207144

| bibcode=2002PASP..114.1124R | s2cid=119453008 | postscript=. }}

}}