3 Puppis

{{Short description|Binary star system in the constellation Puppis}}

{{about-distinguish|l Puppis|j Puppis|L Puppis}}

{{Starbox begin

| name=3 Puppis

}}

{{Starbox image

| image=

{{Location mark

|image=Puppis constellation map.svg|alt=|float=center|width=260

|label=|position=right

|mark=Red circle.svg|mark_width=10|mark_link=3 Pup

|x=451|y=613

}}

|caption=Location of 3 Puppis (circled)

}}{{Starbox observe

| epoch=J2000

| ra={{RA|07|43|48.46872}}{{cite journal|bibcode=2007A&A...474..653V|title=Validation of the new Hipparcos reduction|journal=Astronomy and Astrophysics|volume=474|issue=2|pages=653–664|last1=Van Leeuwen|first1=F.|year=2007|doi=10.1051/0004-6361:20078357|arxiv = 0708.1752 |s2cid=18759600}}

| dec={{DEC|-28|57|17.3720}}

| appmag_v=3.93

| constell=Puppis

}}

{{Starbox character

| class=A2.7Ib{{cite journal|bibcode=2015AstBu..70...99K|arxiv=1502.01444|title=Spectral atlas of A-type supergiants|journal=Astrophysical Bulletin|volume=70|pages=99–108|last1=Klochkova|first1=V. G.|last2=Sendzikas|first2=E. G.|last3=Chentsov|first3=E. L.|year=2015|issue=1|doi=10.1134/S1990341315010113|s2cid=119229144}} {{nowrap|(A2Ia - A3IIpe{{cite journal|bibcode=2010A&A...512A..73M|arxiv=0912.1954|title=Resolving the dusty circumstellar environment of the A[e] supergiant HD 62623 with the VLTI/MIDI|journal=Astronomy and Astrophysics|volume=512|pages=A73|last1=Meilland|first1=A.|last2=Kanaan|first2=S.|last3=Borges Fernandes|first3=M.|last4=Chesneau|first4=O.|last5=Millour|first5=F.|last6=Stee|first6=Ph.|last7=Lopez|first7=B.|year=2010|doi=10.1051/0004-6361/200913640|s2cid=119225591}})}}

| b-v=+0.18{{cite journal|bibcode=1986A&AS...64..205G|title=Low dispersion spectrophotometry of bright early-type stars|journal=Astronomy and Astrophysics Supplement Series|volume=64|pages=205|last1=Gutierrez-Moreno|first1=A.|last2=Moreno|first2=H.|last3=Loyola|first3=P.|last4=Cortes|first4=G.|year=1986}}

| u-b=−0.09

| appmag_1_passband=

| appmag_1=

| appmag_2_passband=

| appmag_2=

| appmag_3_passband=

| appmag_3=

| appmag_4_passband=

| appmag_4=

| appmag_5_passband=K

| appmag_5=2.340{{cite journal|bibcode=2015ApJ...800L..20K|arxiv=1501.07063|title=Discovery of SiO Band Emission from Galactic B[e] Supergiants|journal=The Astrophysical Journal Letters|volume=800|issue=2|pages=L20|last1=Kraus|first1=M.|last2=Oksala|first2=M. E.|last3=Cidale|first3=L. S.|last4=Arias|first4=M. L.|last5=Torres|first5=A. F.|last6=Borges Fernandes|first6=M.|year=2015|doi=10.1088/2041-8205/800/2/L20|s2cid=118847782}}

| variable=

}}

{{Starbox astrometry

| radial_v={{val|26.4|2.0}}

| prop_mo_ra= {{val|-5.09}}

| prop_mo_dec= {{val|+3.90}}

| pm_footnote =

| parallax=0.59

| p_error=0.17

| parallax_footnote=

| dist_ly={{val|{{cvt|630|pc|ly|disp=number}}|{{cvt|85|pc|ly|disp=number}}|fmt=commas}}

| dist_pc={{val|630|85|fmt=commas}}

| dist_footnote=

| absmag_v=−5.5

}}

{{Starbox detail

| source=

| component1 = A

| mass= {{val|8.8|0.5}}

| luminosity= {{val|12600|3300|2600|fmt=commas}}

| gravity= {{val|1.9|0.1}}

| temperature= {{val|8500|500|fmt=commas}}

| radius={{val|54|7}}

| metal=

| rotational_velocity = {{val|35|5}}

| age_myr=

| component2 = B

| mass2 = {{val|0.75|0.25}}

| radius2 = 0.3

| temperature2 = 50,000

| gravity2 = 5.0

}}

{{Starbox orbit

| primary = A

| name = B

| reference =

| period_unitless = {{val|137.4|0.1}} days

| k1 = {{val|5.0|0.8}}

| axis_unitless = {{val|1.11|0.03|ul=AU}}

}}

{{Starbox catalog

| names= l Puppis, GSC 06552-03228, HD 62623, HIP 37677, HR 2996, SAO 174400, CD−28°4774

}}

{{Starbox reference |

Simbad=HIP+37677

}}

{{Starbox end}}

3 Puppis (3 Pup) is a spectroscopic binary in the constellation Puppis. It is a very rare A[e] supergiant, referred to as a B[e] star despite its spectral classification, and its apparent magnitude is 3.93.

3 Puppis is surrounded by a disc of circumstellar dust, which is unusual for an A-type star. It is caused by a low mass companion, a helium-rich subdwarf that is transferring mass to the supergiant. Due to mass transfer, its mass reduced from {{solar mass|3.6}} when it formed to the current {{solar mass|0.75}}.{{Cite journal |last1=Miroshnichenko |first1=A. S. |last2=Danford |first2=S. |last3=Zharikov |first3=S. V. |last4=Klochkova |first4=V. G. |last5=Chentsov |first5=E. L. |last6=Vanbeveren |first6=D. |last7=Zakhozhay |first7=O. V. |last8=Manset |first8=N. |last9=Pogodin |first9=M. A. |last10=Omarov |first10=C. T. |last11=Kuratova |first11=A. K. |last12=Khokhlov |first12=S. A. |date=July 2020 |title=Properties of Galactic B[e] Supergiants. V. 3 Pup–Constraining the Orbital Parameters and Modeling the Circumstellar Environments |journal=The Astrophysical Journal |language=en |volume=897 |issue=1 |pages=48 |doi=10.3847/1538-4357/ab93d9 |doi-access=free |bibcode=2020ApJ...897...48M |issn=0004-637X|arxiv=2005.07754 }} Like most B[e] stars, 3 Pup rotates rapidly, at 20%{{efn|1=Calculated from rotational velocity divided by critical velocity, 35/178 = 0.20.}} of the speed at which it would start to break apart. The disc has its inner edge only 3.8 AU from the primary star and it is suspected that deceleration of the hot primary stellar wind by the companion allows the dust to form unusually close to such a luminous star.