BD+43 3654: Difference between revisions

BD+43 3654
Observation data; Epoch J2000.0 Equinox J2000.0
Constellation	Cygnus
Right ascension	20h 33m 36.079s
Declination	+43° 59′ 07.38″
Apparent magnitude (V)	10.06
Characteristics
Spectral type	O4If
Apparent magnitude (B)	11.245
Apparent magnitude (J)	6.636
Apparent magnitude (H)	6.198
Apparent magnitude (K)	5.973
Astrometry
Proper motion (μ)	RA: 0.5 ± 1.3 mas/yr ; Dec.: 2.0 ± 1.3 mas/yr
Parallax (π)	0.6057 ± 0.0304 mas
Distance	5,400 ± 300 ly ; (1,650 ± 80 pc)
Absolute magnitude (MV)	−6.27
Details
Mass	64.6 M☉
Radius	18.8 R☉
Luminosity (bolometric)	850,000 L☉
Temperature	40,422 K
Age	2.0 Myr
Other designations
	BD+43 3654, GSC 03165-00228, TYC 3165-228-1, 2MASS J20333607+4359075
Database references
SIMBAD	data

Browse history interactively

← Previous edit

Content deleted Content added

VisualWikitext

Inline

Latest revision as of 23:36, 20 October 2024

BD+43 3654 is a massive luminous blue supergiant runaway star in the constellation Cygnus.

Features

BD+43 3654 has a spectral type of O4 If with a mass around 65 times larger than the Sun, likely 850,000 times brighter, and very young, with an age that has been estimated to be around 2 million years. Its distance to the Solar System has been estimated to be 1.45 kiloparsecs (4,700 light-years) and it is moving at high speed through the interstellar medium, creating a bow shock.^[3]

Origin

Studies of the trajectory and speed of BD+43 3654 relative to the other stars of the nearby, massive stellar association Cygnus OB2 suggest it is a runaway star, making it one of the most massive runaway stars known in the Milky Way (along with the O-type supergiants Lambda Cephei and Zeta Puppis).^[3] Initially it was suggested a supernova explosion of a former binary system companion star caused the high velocity of BD+43 3654.^[3]

Later research shows that a supernova ejection would not produce such a high space velocity. Given that BD+43 3654 appears to be younger than most stars in Cygnus OB2, an alternative scenario has been proposed in which BD+43 3654 is a massive blue straggler born in an encounter between two former double stars in the core of Cygnus OB2. In this setting, two stars of each binary would collide and merge forming a larger, more massive star (BD+43 3654), that would be ejected from the stellar association along with two other stars. These additional stars would end by exploding as supernovae to leave behind two pulsars. B2020+28 and B2021+51 are identified as these pulsars, as their dynamics indicate they were expelled from Cygnus OB2.^[6] A derivative consequence of the latter scenario is that the brightest and most massive stars of Cygnus OB2 would be blue stragglers too.

Another theory is that runaways of this mass and velocity can be produced by an encounter between a massive single star and a close binary system. Such an encounter is expected to send the binary system in the opposite direction to the single star, and no such massive binary has been found corresponding to BD+43 3654.^[7]

References

^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j Comerón, F.; Pasquali, A. (2012). "New members of the massive stellar population in Cygnus". Astronomy & Astrophysics. 543: A101. Bibcode:2012A&A...543A.101C. doi:10.1051/0004-6361/201219022. ISSN 0004-6361.
^ ^a ^b ^c Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862.
^ ^a ^b ^c ^d Comerón, F.; Pasquali, A. (2007). "A very massive runaway star from Cygnus OB2". Astronomy & Astrophysics. 467 (1): L23 – L27. arXiv:0704.0676. Bibcode:2007A&A...467L..23C. doi:10.1051/0004-6361:20077304. S2CID 16843959.
^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
^ Hillier, D. J.; Schaerer, D.; Martins, F. (2005). "A new calibration of stellar parameters of Galactic O stars". Astronomy & Astrophysics. 436 (3): 1049–1065. arXiv:astro-ph/0503346. Bibcode:2005A&A...436.1049M. doi:10.1051/0004-6361:20042386. S2CID 39162419.
^ Gvaramadze, V. V.; Bomans, D. J. (2008). "BD+43 3654 - a blue straggler?". Astronomy & Astrophysics. 485 (3): L29 – L32. arXiv:0805.3893. Bibcode:2008A&A...485L..29G. doi:10.1051/0004-6361:200809860. S2CID 18755032.
^ Gvaramadze, Vasilii V.; Gualandris, Alessia (2011). "Very massive runaway stars from three-body encounters". Monthly Notices of the Royal Astronomical Society. 410 (1): 304–312. arXiv:1007.5057. Bibcode:2011MNRAS.410..304G. doi:10.1111/j.1365-2966.2010.17446.x. S2CID 123481910.

[comeron2012-1] ^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j Comerón, F.; Pasquali, A. (2012). "New members of the massive stellar population in Cygnus". Astronomy & Astrophysics. 543: A101. Bibcode:2012A&A...543A.101C. doi:10.1051/0004-6361/201219022. ISSN 0004-6361.

[tycho2-2] Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862.

[Comeron2007-3] Comerón, F.; Pasquali, A. (2007). "A very massive runaway star from Cygnus OB2". Astronomy & Astrophysics. 467 (1): L23 – L27. arXiv:0704.0676. Bibcode:2007A&A...467L..23C. doi:10.1051/0004-6361:20077304. S2CID 16843959.

[dr2-4] Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.

[Hillier2005-5] Hillier, D. J.; Schaerer, D.; Martins, F. (2005). "A new calibration of stellar parameters of Galactic O stars". Astronomy & Astrophysics. 436 (3): 1049–1065. arXiv:astro-ph/0503346. Bibcode:2005A&A...436.1049M. doi:10.1051/0004-6361:20042386. S2CID 39162419.

[Gvaramadze2008-6] Gvaramadze, V. V.; Bomans, D. J. (2008). "BD+43 3654 - a blue straggler?". Astronomy & Astrophysics. 485 (3): L29 – L32. arXiv:0805.3893. Bibcode:2008A&A...485L..29G. doi:10.1051/0004-6361:200809860. S2CID 18755032.

[7] Gvaramadze, Vasilii V.; Gualandris, Alessia (2011). "Very massive runaway stars from three-body encounters". Monthly Notices of the Royal Astronomical Society. 410 (1): 304–312. arXiv:1007.5057. Bibcode:2011MNRAS.410..304G. doi:10.1111/j.1365-2966.2010.17446.x. S2CID 123481910.

[1]

[2]

[3]

[4]

[5]

[6]

[7]

@@ Line 1: / Line 1: @@
+{{Short description|Star in the constellation Cygnus}}
 {{Starbox begin
-| name = BD+43° 3654
+| name = BD+43 3654
-}}
+}}<!--
 {{Starbox image
 | image =
 | caption =
 }}
-{{Starbox observe
+-->{{Starbox observe
 | epoch = [[J2000.0]]
 | equino = [[J2000.0]]
 | constell = [[Cygnus (constellation)|Cygnus]]
 | pronounce =
-| ra = {{RA|20|33|36.079}}<ref name=comeron2012>{{cite journal|last1=Comerón|first1=F.|last2=Pasquali|first2=A.|title=New members of the massive stellar population in Cygnus|journal=Astronomy & Astrophysics|volume=543|year=2012|pages=A101|issn=0004-6361|doi=10.1051/0004-6361/201219022|bibcode = 2012A&A...543A.101C }}</ref>
+| ra = {{RA|20|33|36.079}}<ref name=comeron2012>{{cite journal|last1=Comerón|first1=F.|last2=Pasquali|first2=A.|title=New members of the massive stellar population in Cygnus|journal=Astronomy & Astrophysics|volume=543|year=2012|pages=A101|issn=0004-6361|doi=10.1051/0004-6361/201219022|bibcode = 2012A&A...543A.101C |doi-access=free}}</ref>
 | dec = {{DEC|+43|59|07.38}}<ref name=comeron2012/>
 | appmag_v = 10.06<ref name=tycho2/>
@@ Line 27: / Line 28: @@
 | journal = Astronomy & Astrophysics
 | year = 2007
+| issue = 1
 |bibcode = 2007A&A...467L..23C
 | doi = 10.1051/0004-6361:20077304
-|arxiv = 0704.0676 }}</ref>
+|arxiv = 0704.0676 | s2cid = 16843959
+}}</ref>
 | appmag_1_passband = B
 | appmag_1 = 11.245<ref name=comeron2012/>
@@ Line 56: / Line 59: @@
 {{Starbox astrometry
  | radial_v =
- | prop_mo_ra = {{nowrap|0.5 ± 1.3<ref name=tycho2>{{cite journal|bibcode=2000A&A...355L..27H|title=The Tycho-2 catalogue of the 2.5 million brightest stars|journal=Astronomy and Astrophysics|volume=355|pages=L27|author1=Høg|first1=E.|last2=Fabricius|first2=C.|last3=Makarov|first3=V. V.|last4=Urban|first4=S.|last5=Corbin|first5=T.|last6=Wycoff|first6=G.|last7=Bastian|first7=U.|last8=Schwekendiek|first8=P.|last9=Wicenec|first9=A.|year=2000}}</ref>}}
+ | prop_mo_ra = {{nowrap|0.5 ± 1.3<ref name=tycho2>{{cite journal|bibcode=2000A&A...355L..27H|title=The Tycho-2 catalogue of the 2.5 million brightest stars|journal=Astronomy and Astrophysics|volume=355|pages=L27|last1=Høg|first1=E.|last2=Fabricius|first2=C.|last3=Makarov|first3=V. V.|last4=Urban|first4=S.|last5=Corbin|first5=T.|last6=Wycoff|first6=G.|last7=Bastian|first7=U.|last8=Schwekendiek|first8=P.|last9=Wicenec|first9=A.|year=2000|doi=10.1888/0333750888/2862}}</ref>}}
  | prop_mo_dec = {{nowrap|2.0 ± 1.3<ref name=tycho2/>}}
- | parallax = 0.40
+ | parallax = 0.6057
- | p_error = 0.64
+ | p_error = 0.0304
+ | parallax_footnote = <ref name=dr2>{{cite DR2|2069819545390584192}}</ref>
- | parallax_footnote = <ref name=dr1>{{cite journal|bibcode=2016yCat.1337....0G|title=VizieR Online Data Catalog: Gaia DR1 (Gaia Collaboration, 2016)|journal=VizieR On-line Data Catalog: I/337.  Originally published in: Astron. Astrophys|volume=1337|author1=Gaia Collaboration|year=2016}}</ref>
+ | dist_ly =
- | dist_ly = 4,700
+ | dist_pc =
- | dist_pc = 1,450<ref name=Comeron2007/>
  | absmag_v = &minus;6.27<ref name=comeron2012/>
  }}
@@ Line 69: / Line 71: @@
 | source              =
 | mass                = 64.6<ref name=comeron2012/>
-| radius              =
+| radius              = 18.8
 | gravity             =
 | luminosity          =
@@ Line 88: / Line 90: @@
 |bibcode = 2005A&A...436.1049M
 | doi = 10.1051/0004-6361:20042386
-|arxiv = astro-ph/0503346 }}</ref>
+|arxiv = astro-ph/0503346 | s2cid = 39162419
+}}</ref>
 | luminosity_visual   =
 | temperature         = 40,422<ref name=comeron2012/>
@@ Line 98: / Line 101: @@
 }}
 {{Starbox catalog
-| names = [[Bonner Durchmusterung|BD]]+43°&nbsp;3654, [[Guide Star Catalogue|GSC]]&nbsp;03165-00228, [[Tycho Catalogue|TYC]]&nbsp;3165-228-1, [[2MASS]]&nbsp;J20333607+4359075
+| names = [[Bonner Durchmusterung|BD]]+43&nbsp;3654, [[Guide Star Catalogue|GSC]]&nbsp;03165-00228, [[Tycho Catalogue|TYC]]&nbsp;3165-228-1, [[2MASS]]&nbsp;J20333607+4359075
 }}
 {{Starbox reference
@@ Line 105: / Line 108: @@
 {{Starbox end}}
-'''[[Bonner Durchmusterung|BD]]+43° 3654''' is a massive luminous [[blue supergiant]] [[runaway star]] in the [[constellation]] [[Cygnus (constellation)|Cygnus]].
+'''BD+43 3654''' is a massive luminous [[blue supergiant]] [[runaway star]] in the [[constellation]] [[Cygnus (constellation)|Cygnus]].
 ==Features==
-BD+43° 3654 has a [[spectral classification|spectral type]] of [[Stellar classification#Class O|O4]][[supergiant|I]]f with a mass around 70 times larger than the Sun, likely 850,000 times brighter, and very young, with an age that has been estimated to be around 2 million years. Its distance to the [[Solar System]] has been estimated to be 1.45 kilo[[parsec]]s (4,700 [[light-year]]s) and it is moving at high speed through the [[interstellar medium]], creating a [[shockwave|bow shock]].<ref name=Comeron2007/>
+BD+43 3654 has a [[spectral classification|spectral type]] of [[Stellar classification#Class O|O4]][[supergiant|I]]f with a mass around 65 times larger than the Sun, likely 850,000 times brighter, and very young, with an age that has been estimated to be around 2 million years. Its distance to the [[Solar System]] has been estimated to be 1.45 kilo[[parsec]]s (4,700 [[light-year]]s) and it is moving at high speed through the [[interstellar medium]], creating a [[shockwave|bow shock]].<ref name=Comeron2007/>
 ==Origin==
-Studies of the trajectory and speed of BD+43° 3654 relative to the other stars of the nearby, massive [[stellar association]] [[Cygnus OB2]] suggest it is a [[runaway star]], making it one of the most massive runaway stars known in the [[Milky Way]] (along with the O-type supergiants [[Lambda Cephei]] and [[Zeta Puppis]]).<ref name=Comeron2007/>  Initially it was suggested a [[supernova]] explosion of a former [[binary system]] companion star caused the high velocity of BD+43° 3654.<ref name=Comeron2007/>
+Studies of the trajectory and speed of BD+43 3654 relative to the other stars of the nearby, massive [[stellar association]] [[Cygnus OB2]] suggest it is a [[runaway star]], making it one of the most massive runaway stars known in the [[Milky Way]] (along with the O-type supergiants [[Lambda Cephei]] and [[Zeta Puppis]]).<ref name=Comeron2007/>  Initially it was suggested a [[supernova]] explosion of a former [[binary system]] companion star caused the high velocity of BD+43 3654.<ref name=Comeron2007/>
-Later research shows that a supernova ejection would not produce such a high [[space velocity (astronomy)|space velocity]]. Given that BD+43° 3654 appears to be younger than most stars in Cygnus OB2, an alternative scenario has been proposed in which BD+43° 3654 is a massive [[blue straggler]] born in an encounter between two former double stars in the core of Cygnus OB2. In this setting, two stars of each binary would collide and merge forming a larger, more massive star (BD+43° 3654), that would be ejected from the stellar association along with two other stars. These additional stars would end by exploding as supernovae to leave behind two [[pulsar]]s. B2020+28 and B2021+51-, are identified as these pulsars, as their dynamics indicate they were expelled from Cygnus OB2.<ref name=Gvaramadze2008>
+Later research shows that a supernova ejection would not produce such a high [[space velocity (astronomy)|space velocity]]. Given that BD+43 3654 appears to be younger than most stars in Cygnus OB2, an alternative scenario has been proposed in which BD+43 3654 is a massive [[blue straggler]] born in an encounter between two former double stars in the core of Cygnus OB2. In this setting, two stars of each binary would collide and merge forming a larger, more massive star (BD+43 3654), that would be ejected from the stellar association along with two other stars. These additional stars would end by exploding as supernovae to leave behind two [[pulsar]]s. B2020+28 and B2021+51 are identified as these pulsars, as their dynamics indicate they were expelled from Cygnus OB2.<ref name=Gvaramadze2008>
 {{cite journal
 | volume = 485
@@ Line 122: / Line 125: @@
 | last2 = Bomans
 | first2 = D. J.
-| title = BD+43° 3654 - a blue straggler?
+| title = BD+43 3654 - a blue straggler?
 | journal = Astronomy & Astrophysics
 | year = 2008
 |bibcode = 2008A&A...485L..29G
 | doi = 10.1051/0004-6361:200809860
-|arxiv = 0805.3893 }}</ref> A derivative consequence of the latter scenario is that the brightest and most massive stars of Cygnus OB2 would be blue stragglers too.
+|arxiv = 0805.3893 | s2cid = 18755032
+}}</ref> A derivative consequence of the latter scenario is that the brightest and most massive stars of Cygnus OB2 would be blue stragglers too.
-Another theory is that runaways of this mass and velocity can be produced by an encounter between a massive single star and a close binary system.  Such an encounter is expected to send the binary system in the opposite direction to the single star, and no such massive binary has been found corresponding to BD+43° 3654.<ref>{{cite journal|bibcode=2011MNRAS.410..304G|arxiv=1007.5057|title=Very massive runaway stars from three-body encounters|journal=Monthly Notices of the Royal Astronomical Society|volume=410|pages=304|author1=Gvaramadze|first1=Vasilii V.|last2=Gualandris|first2=Alessia|year=2011|doi=10.1111/j.1365-2966.2010.17446.x}}</ref>
+Another theory is that runaways of this mass and velocity can be produced by an encounter between a massive single star and a close binary system.  Such an encounter is expected to send the binary system in the opposite direction to the single star, and no such massive binary has been found corresponding to BD+43 3654.<ref>{{cite journal|bibcode=2011MNRAS.410..304G|arxiv=1007.5057|title=Very massive runaway stars from three-body encounters|journal=Monthly Notices of the Royal Astronomical Society|volume=410|pages=304–312|last1=Gvaramadze|first1=Vasilii V.|last2=Gualandris|first2=Alessia|year=2011|issue=1|doi=10.1111/j.1365-2966.2010.17446.x|doi-access=free |s2cid=123481910 }}</ref>
+==See also ==
+* [[List of most massive stars]]
 ==References==
@@ Line 137: / Line 145: @@
 {{DEFAULTSORT:BD 43 3654}}
-[[Category:Cygnus (constellation)]]
 [[Category:O-type supergiants]]
-[[Category:Durchmusterung objects|BD 43 3654]]
 [[Category:Emission-line stars]]
+[[Category:Blue stragglers]]
 [[Category:Runaway stars]]
-[[Category:2MASS objects]]
+[[Category:Cygnus (constellation)]]
+[[Category:Durchmusterung objects|BD 43 3654]]
+[[Category:2MASS objects|J20333607+4359075]]

Observation data Epoch J2000.0 Equinox J2000.0
Constellation	Cygnus
Right ascension	20^h 33^m 36.079^s^[1]
Declination	+43° 59′ 07.38″^[1]
Apparent magnitude (V)	10.06^[2]
Characteristics
Spectral type	O4If^[3]
Apparent magnitude (B)	11.245^[1]
Apparent magnitude (J)	6.636^[1]
Apparent magnitude (H)	6.198^[1]
Apparent magnitude (K)	5.973^[1]
Astrometry

Proper motion (μ)	RA: 0.5 ± 1.3^[2] mas/yr Dec.: 2.0 ± 1.3^[2] mas/yr
Parallax (π)	0.6057 ± 0.0304 mas^[4]
Distance	5,400 ± 300 ly (1,650 ± 80 pc)
Absolute magnitude (M_V)	−6.27^[1]

Details

Mass	64.6^[1] `M`_☉
Radius	18.8 `R`_☉
Luminosity (bolometric)	850,000^[5] `L`_☉
Temperature	40,422^[1] K
Age	2.0^[1] Myr

Other designations
BD+43 3654, GSC 03165-00228, TYC 3165-228-1, 2MASS J20333607+4359075
Database references
SIMBAD	data