Astronomy:HD 101584: Difference between revisions

From HandWiki
(change)
 
(simplify)
 
Line 4: Line 4:
}}
}}
{{Starbox image
{{Starbox image
|image=[[File:HD 101584.jpg|250px]]
|image=250px
|caption=HD 101584 seen by [[Astronomy:Atacama Large Millimeter Array|ALMA]]. The blue component moves towards the observer and the red component moves away from the observer. The green component has the same speed as the binary system, seen as a green point source in the middle.
|caption=HD 101584 seen by [[Astronomy:Atacama Large Millimeter Array|ALMA]]. The blue component moves towards the observer and the red component moves away from the observer. The green component has the same speed as the binary system, seen as a green point source in the middle.
|credit=ALMA (ESO/NAOJ/NRAO), Olofsson et al.<br />Acknowledgement: Robert Cumming
|credit=ALMA (ESO/NAOJ/NRAO), Olofsson et al.<br />Acknowledgement: Robert Cumming
Line 44: Line 44:
{{Starbox end}}
{{Starbox end}}


'''HD 101584''' is a suspected [[Astronomy:Post common envelope binary|post-common envelope binary]] about 1,800 to 5,900 [[Astronomy:Light-year|light-year]]s distant in the constellation of [[Astronomy:Centaurus|Centaurus]].<ref name="Olofsson et al">{{Cite journal|last1=Olofsson|first1=H.|last2=Khouri|first2=T.|last3=Maercker|first3=M.|last4=Bergman|first4=P.|last5=Doan|first5=L.|last6=Tafoya|first6=D.|last7=Vlemmings|first7=W. H. T.|last8=Humphreys|first8=E. M. L.|last9=Lindqvist|first9=M.|last10=Nyman|first10=L.|last11=Ramstedt|first11=S.|date=March 2019|title=HD 101584: circumstellar characteristics and evolutionary status|journal= Astronomy & Astrophysics|language=en|volume=623|pages=A153|doi=10.1051/0004-6361/201834897|issn=0004-6361|bibcode=2019A&A...623A.153O|arxiv=1902.02153|s2cid=102480818}}</ref><ref name="ALMA press">{{Cite web|url=https://www.almaobservatory.org/en/audiences/alma-catches-beautiful-outcome-of-stellar-fight/|title=ALMA catches beautiful outcome of stellar fight|website=Atacama Large Millimeter/submillimeter Array}}</ref> The system is bright at optical wavelengths with an [[Astronomy:Apparent visual magnitude|apparent visual magnitude]] of about 7. The primary is either a post-AGB star, but more likely a post-[[Astronomy:Red-giant branch|RGB]] star. The secondary is a [[Astronomy:Red dwarf|red dwarf]] or possibly a low-luminosity [[Astronomy:White dwarf|white dwarf]], which orbits the primary every 150-200 days. The system is surrounded by a slowly rotating [[Astronomy:Circumstellar disc#Binary system|circumbinary disk]], probably with a face-on orientation towards the solar system and a size of about 150 [[Astronomy:Astronomical unit|astronomical unit]]s.<ref name="Olofsson et al"/>
'''HD 101584''' is a suspected [[Astronomy:Post common envelope binary|post-common envelope binary]] about 1,800 to 5,900 [[Astronomy:Light-year|light-year]]s distant in the constellation of [[Astronomy:Centaurus|Centaurus]].<ref name="Olofsson et al">{{Cite journal|last1=Olofsson|first1=H.|last2=Khouri|first2=T.|last3=Maercker|first3=M.|last4=Bergman|first4=P.|last5=Doan|first5=L.|last6=Tafoya|first6=D.|last7=Vlemmings|first7=W. H. T.|last8=Humphreys|first8=E. M. L.|last9=Lindqvist|first9=M.|last10=Nyman|first10=L.|last11=Ramstedt|first11=S.|date=March 2019|title=HD 101584: circumstellar characteristics and evolutionary status|journal= Astronomy & Astrophysics|language=en|volume=623|pages=A153|doi=10.1051/0004-6361/201834897|issn=0004-6361|bibcode=2019A&A...623A.153O|arxiv=1902.02153|s2cid=102480818}}</ref><ref name="ALMA press">{{Cite web|url=https://www.almaobservatory.org/en/audiences/alma-catches-beautiful-outcome-of-stellar-fight/|title=ALMA catches beautiful outcome of stellar fight|website=Atacama Large Millimeter/submillimeter Array}}</ref> The system is bright at optical wavelengths with an [[Astronomy:Apparent visual magnitude|apparent visual magnitude]] of about 7. The primary is either a post-AGB star, but more likely a post-[[Astronomy:Red-giant branch|RGB]] star. The secondary is a [[Astronomy:Red dwarf|red dwarf]] or possibly a low-luminosity [[Astronomy:White dwarf|white dwarf]], which orbits the primary every 150-200 days. The system is surrounded by a slowly rotating [[Astronomy:Circumstellar disc#Binary system|circumbinary disk]], probably with a face-on orientation towards the [[Astronomy:Solar System|Solar System]] and a size of about 150 [[Astronomy:Astronomical unit|astronomical unit]]s.<ref name="Olofsson et al"/>


== Variability ==
== Variability ==
[[File:V885CenLightCurve.png|thumb|left|A [[Astronomy:Light curve|light curve]] for V885 Centauri, plotted from ''Hipparcos'' data<ref name="CDS">{{cite web | url=https://cdsarc.cds.unistra.fr/viz-bin/ftp-index?/ftp/cats/more/HIP/cdroms/cats | website=Centre de Données astronomiques de Strasbourg | title=/ftp/cats/more/HIP/cdroms/cats | publisher=Strasbourg astronomical Data Center |access-date=15 October 2022}}</ref>]]
[[File:V885CenLightCurve.png|thumb|left|A [[light curve]] for V885 Centauri, plotted from ''Hipparcos'' data<ref name="CDS">{{cite web | url=https://cdsarc.cds.unistra.fr/viz-bin/ftp-index?/ftp/cats/more/HIP/cdroms/cats | website=Centre de Données astronomiques de Strasbourg | title=/ftp/cats/more/HIP/cdroms/cats | publisher=Strasbourg astronomical Data Center |access-date=15 October 2022}}</ref>]]
In 1991, Jean Manfroid ''et al.'' published [[Astronomy:Photometry|photometry]] that showed that HD 101584 is a [[Astronomy:Variable star|variable star]].<ref name="Manfroid1991">{{cite journal |last1=Manfroid |first1=J. |last2=Sterken |first2=C. |last3=Bruch |first3=A. |last4=Burger |first4=M. |last5=de Groot |first5=M. |last6=Duerbeck |first6=H. W. |last7=Duemmler |first7=R. |last8=Figer |first8=A. |last9=Hageman |first9=T. |last10=Hensberge |first10=H. |last11=Jorissen |first11=A. |last12=Madejsky |first12=R. |last13=Mandel |first13=H. |last14=Ott |first14=H. A. |last15=Reitermann |first15=A. |last16=Schulte-Ladbeck |first16=R. E. |last17=Stahl |first17=O. |last18=Steenman |first18=H. |last19=Vander Linden |first19=D. |last20=Zickgraf |first20=F. J. |title=Long-term photometry of variables at ESO. I. The first data catalogue (1982-1986) |journal=Astronomy and Astrophysics, Suppl. Ser. |date=March 1991 |volume=87 |pages=481-498 | bibcode=1991A&AS...87..481M |url=https://articles.adsabs.harvard.edu/pdf/1991A%26AS...87..481M |access-date=20 January 2025}}</ref>
HD 101584 has been given the [[Astronomy:Variable star designation|variable star designation]] V885 Centauri.  The International Variable Star Index states that the star varies between visual magnitude 6.90 and 7.02, over a period of 87.9 days.<ref name="IVSI">{{cite web |title=V0885 Cen |url=https://www.aavso.org/vsx/index.php?view=detail.top&oid=8182 |website=The International Variable Star Index |publisher=AAVSO |access-date=21 October 2022}}</ref> However Koen and Eyer detected, in the star's ''[[Astronomy:Hipparcos|Hipparcos]]'' data, an oscillation of the star's brightness with a period of 6.744 days and an amplitude of only 0.02 magnitudes.<ref name="Koen">{{cite journal |last1=Koen |first1=Chris |last2=Eyer |first2=Laurent |title=New periodic variables from the Hipparcos epoch photometry |journal=Monthly Notices of the Royal Astronomical Society |date=March 2002 |volume=331 |issue=1 |pages=45–59 |doi=10.1046/j.1365-8711.2002.05150.x |arxiv=astro-ph/0112194 |bibcode=2002MNRAS.331...45K |doi-access=free }}</ref>
HD 101584 has been given the [[Astronomy:Variable star designation|variable star designation]] V885 Centauri.  The International Variable Star Index states that the star varies between visual magnitude 6.90 and 7.02, over a period of 87.9 days.<ref name="IVSI">{{cite web |title=V0885 Cen |url=https://www.aavso.org/vsx/index.php?view=detail.top&oid=8182 |website=The International Variable Star Index |publisher=AAVSO |access-date=21 October 2022}}</ref> However Koen and Eyer detected, in the star's ''[[Astronomy:Hipparcos|Hipparcos]]'' data, an oscillation of the star's brightness with a period of 6.744 days and an amplitude of only 0.02 magnitudes.<ref name="Koen">{{cite journal |last1=Koen |first1=Chris |last2=Eyer |first2=Laurent |title=New periodic variables from the Hipparcos epoch photometry |journal=Monthly Notices of the Royal Astronomical Society |date=March 2002 |volume=331 |issue=1 |pages=45–59 |doi=10.1046/j.1365-8711.2002.05150.x |arxiv=astro-ph/0112194 |bibcode=2002MNRAS.331...45K |doi-access=free }}</ref>
{{clear left}}
{{clear left}}


== Nebula ==
== Nebula ==
[[File:HD 101584 Hubble.jpg|thumb|left|HD 101584 and the surrounding nebula, seen by [[Astronomy:Hubble Space Telescope|Hubble]]]]
[[File:HD 101584 Hubble.jpg|thumb|left|HD 101584 and the surrounding nebula, seen by [[Hubble Space Telescope|Hubble]]]]
The [[Astronomy:Hubble Space Telescope|Hubble Space Telescope]] image shows a diffuse [[Astronomy:Circumstellar disc|circumstellar]] environment with a circular ring around HD 101584. [[Astronomy:Atacama Large Millimeter Array|ALMA]] mapped the nebula around HD 101584 and was able to map the region close to the central binary. The nebula consists of a central compact source, an equatorial density enhancement (disk), a high-velocity bipolar outflow and an hourglass structure surrounding the outflow. The outflow reaches a maximum velocity of about 150 km/s and is inclined to the line of sight by {{val|10|10|5}}[[Degree (angle)|°]]. There is evidence for a second bipolar outflow with a different orientation from the major outflow.<ref name="Olofsson et al"/> The inner disk, heated to 1540 [[Kelvin|K]], currently has been sublimated by the increasing luminosity of the star.<ref>{{citation|arxiv=2008.11555|year=2020|title=VLTI/PIONIER reveals the close environment of the evolved system HD 101584|doi=10.1051/0004-6361/202037946 |last1=Kluska |first1=J. |last2=Olofsson |first2=H. |last3=Van Winckel |first3=H. |last4=Khouri |first4=T. |last5=Wittkowski |first5=M. |last6=De Wit |first6=W. J. |last7=Humphreys |first7=E. M. L. |last8=Lindqvist |first8=M. |last9=Maercker |first9=M. |last10=Ramstedt |first10=S. |last11=Tafoya |first11=D. |last12=Vlemmings |first12=W. H. T. |journal=Astronomy & Astrophysics |volume=642 |pages=A152 |bibcode=2020A&A...642A.152K |s2cid=221319788 }}</ref>
The [[Astronomy:Hubble Space Telescope|Hubble Space Telescope]] image shows a diffuse [[Astronomy:Circumstellar disc|circumstellar]] environment with a circular ring around HD 101584. [[Astronomy:Atacama Large Millimeter Array|ALMA]] mapped the nebula around HD 101584 and was able to map the region close to the central binary. The nebula consists of a central compact source, an equatorial density enhancement (disk), a high-velocity bipolar outflow and an hourglass structure surrounding the outflow. The outflow reaches a maximum velocity of about 150 km/s and is inclined to the line of sight by {{val|10|10|5}}[[Degree (angle)|°]]. There is evidence for a second bipolar outflow with a different orientation from the major outflow.<ref name="Olofsson et al"/> The inner disk, heated to 1540 [[Kelvin|K]], currently has been sublimated by the increasing luminosity of the star.<ref>{{citation|arxiv=2008.11555|year=2020|title=VLTI/PIONIER reveals the close environment of the evolved system HD 101584|doi=10.1051/0004-6361/202037946 |last1=Kluska |first1=J. |last2=Olofsson |first2=H. |last3=Van Winckel |first3=H. |last4=Khouri |first4=T. |last5=Wittkowski |first5=M. |last6=De Wit |first6=W. J. |last7=Humphreys |first7=E. M. L. |last8=Lindqvist |first8=M. |last9=Maercker |first9=M. |last10=Ramstedt |first10=S. |last11=Tafoya |first11=D. |last12=Vlemmings |first12=W. H. T. |journal=Astronomy & Astrophysics |volume=642 |pages=A152 |bibcode=2020A&A...642A.152K |s2cid=221319788 }}</ref>


Line 65: Line 66:
{{DEFAULTSORT:HD 101584}}
{{DEFAULTSORT:HD 101584}}
[[Category:Binary stars]]
[[Category:Binary stars]]
[[Category:Nebulae]]
[[Category:Protoplanetary nebulae]]
[[Category:Protoplanetary nebulae]]
[[Category:Objects with variable star designations|Centauri, V885]]
[[Category:Objects with variable star designations|Centauri, V885]]

Latest revision as of 17:31, 28 July 2025

Short description: Star in the constellation Centaurus
HD 101584
250px
HD 101584 seen by ALMA. The blue component moves towards the observer and the red component moves away from the observer. The green component has the same speed as the binary system, seen as a green point source in the middle.
Credit: ALMA (ESO/NAOJ/NRAO), Olofsson et al.
Acknowledgement: Robert Cumming
Observation data
Equinox J2000.0]] (ICRS)
Constellation Centaurus
Right ascension  11h 40m 58.80515s[1]
Declination −55° 34′ 25.8147″[1]
Apparent magnitude (V) 7.01
Characteristics
Spectral type A6Ia[2]
Astrometry
Proper motion (μ) RA: −7.935[1] mas/yr
Dec.: −0.243[1] mas/yr
Parallax (π)0.5452 ± 0.0199[1] mas
Distance6,000 ± 200 ly
(1,830 ± 70 pc)
Details
supergiant
Mass0.5 - 1[3] M☉
Radius18.6[3] R☉
Luminosity1,600 L☉ (@1kpc) (400 - 5,000)[3] L☉
Temperature8,500[4] K
companion
Mass0.27 - 0.41[3] M☉
Other designations
IRAS 11385-5517, V885 Centauri, HIP 56992, 2MASS J11405880-5534258
Database references
SIMBADdata

HD 101584 is a suspected post-common envelope binary about 1,800 to 5,900 light-years distant in the constellation of Centaurus.[3][5] The system is bright at optical wavelengths with an apparent visual magnitude of about 7. The primary is either a post-AGB star, but more likely a post-RGB star. The secondary is a red dwarf or possibly a low-luminosity white dwarf, which orbits the primary every 150-200 days. The system is surrounded by a slowly rotating circumbinary disk, probably with a face-on orientation towards the Solar System and a size of about 150 astronomical units.[3]

Variability

A light curve for V885 Centauri, plotted from Hipparcos data[6]

In 1991, Jean Manfroid et al. published photometry that showed that HD 101584 is a variable star.[7] HD 101584 has been given the variable star designation V885 Centauri. The International Variable Star Index states that the star varies between visual magnitude 6.90 and 7.02, over a period of 87.9 days.[8] However Koen and Eyer detected, in the star's Hipparcos data, an oscillation of the star's brightness with a period of 6.744 days and an amplitude of only 0.02 magnitudes.[9]

Nebula

HD 101584 and the surrounding nebula, seen by Hubble

The Hubble Space Telescope image shows a diffuse circumstellar environment with a circular ring around HD 101584. ALMA mapped the nebula around HD 101584 and was able to map the region close to the central binary. The nebula consists of a central compact source, an equatorial density enhancement (disk), a high-velocity bipolar outflow and an hourglass structure surrounding the outflow. The outflow reaches a maximum velocity of about 150 km/s and is inclined to the line of sight by 10+10
−5°. There is evidence for a second bipolar outflow with a different orientation from the major outflow.[3] The inner disk, heated to 1540 K, currently has been sublimated by the increasing luminosity of the star.[10]

Evolution

The companion of this system was captured a few hundred years ago, for example when the red giant reached its critical size. It spiralled towards the red giant but stopped before it merged with the core of the primary. During this stage the outer layers of the red giant were ejected. During the common envelope phase the red giant phase of the primary was terminated and the core was revealed.[3] Later, the bipolar jets formed and met the ejected material, forming the hourglass-shaped structure.[5] Ejected material shows prominent spectral features of magnesium,[11] while outer ejected structures contain methanol and formaldehyde.[12]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ Sivarani, T.; Parthasarathy, M.; García-Lario, P.; Manchado, A.; Pottasch, S. R. (June 1999). "Spectroscopy of the post-AGB star HD 101584 (IRAS 11385-5517)" (in en). Astronomy and Astrophysics Supplement Series 137 (3): 505–519. doi:10.1051/aas:1999259. ISSN 0365-0138. Bibcode: 1999A&AS..137..505S. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 Olofsson, H.; Khouri, T.; Maercker, M.; Bergman, P.; Doan, L.; Tafoya, D.; Vlemmings, W. H. T.; Humphreys, E. M. L. et al. (March 2019). "HD 101584: circumstellar characteristics and evolutionary status" (in en). Astronomy & Astrophysics 623: A153. doi:10.1051/0004-6361/201834897. ISSN 0004-6361. Bibcode: 2019A&A...623A.153O. 
  4. ↑ Olofsson, H.; Black, J. H.; Khouri, T.; Vlemmings, W. H. T.; Humphreys, E. M. L.; Lindqvist, M.; Maercker, M.; Nyman, L. et al. (2021). "Heavy-element Rydberg transition line emission from the post-giant-evolution star HD 101584". Astronomy and Astrophysics 651: A35. doi:10.1051/0004-6361/202140537. Bibcode: 2021A&A...651A..35O. 
  5. ↑ 5.0 5.1 "ALMA catches beautiful outcome of stellar fight". https://www.almaobservatory.org/en/audiences/alma-catches-beautiful-outcome-of-stellar-fight/. 
  6. ↑ "/ftp/cats/more/HIP/cdroms/cats". Strasbourg astronomical Data Center. https://cdsarc.cds.unistra.fr/viz-bin/ftp-index?/ftp/cats/more/HIP/cdroms/cats. 
  7. ↑ Manfroid, J.; Sterken, C.; Bruch, A.; Burger, M.; de Groot, M.; Duerbeck, H. W.; Duemmler, R.; Figer, A. et al. (March 1991). "Long-term photometry of variables at ESO. I. The first data catalogue (1982-1986)". Astronomy and Astrophysics, Suppl. Ser. 87: 481-498. Bibcode: 1991A&AS...87..481M. https://articles.adsabs.harvard.edu/pdf/1991A%26AS...87..481M. Retrieved 20 January 2025. 
  8. ↑ "V0885 Cen". AAVSO. https://www.aavso.org/vsx/index.php?view=detail.top&oid=8182. 
  9. ↑ Koen, Chris; Eyer, Laurent (March 2002). "New periodic variables from the Hipparcos epoch photometry". Monthly Notices of the Royal Astronomical Society 331 (1): 45–59. doi:10.1046/j.1365-8711.2002.05150.x. Bibcode: 2002MNRAS.331...45K. 
  10. ↑ Kluska, J.; Olofsson, H.; Van Winckel, H.; Khouri, T.; Wittkowski, M.; De Wit, W. J.; Humphreys, E. M. L.; Lindqvist, M. et al. (2020), "VLTI/PIONIER reveals the close environment of the evolved system HD 101584", Astronomy & Astrophysics 642: A152, doi:10.1051/0004-6361/202037946, Bibcode: 2020A&A...642A.152K 
  11. ↑ Heavy-element Rydberg transition line emission from the post-giant-evolution star HD 101584
  12. ↑ Basalgète, R.; Dupuy, R.; Féraud, G.; Romanzin, C.; Philippe, L.; Michaut, X.; Michoud, J.; Amiaud, L. et al. (2021), "Complex organic molecules in protoplanetary disks: X-ray photodesorption from methanol-containing ices", Astronomy & Astrophysics 647: A35, doi:10.1051/0004-6361/202039676 



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:HD_101584&oldid=3741700"