L2 Puppis

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L2 Puppis
Puppis constellation map.svg
Red circle.svg
Location of L2 Puppis (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Puppis
Right ascension 07h 13m 32.31810s [1]
Declination −44° 38′ 23.0630″ [1]
Apparent magnitude  (V)5.10 [2]
2.6–6 (GCVS) [3]
6–8 (1995 – ) [4]
Characteristics
Evolutionary stage Red-giant branch [5]
Spectral type M5IIIe [3]
U−B color index +1.24 [2]
B−V color index +1.56 [2]
Variable type SRb [3]
Astrometry
Radial velocity (Rv)33.0 [6]  km/s
Proper motion (μ)RA: 106.31 [1]   mas/yr
Dec.: 324.99 [1]   mas/yr
Parallax (π)15.61 ± 0.99  mas [1]
Distance 210 ± 10  ly
(64 ± 4  pc)
Details
Mass 0.659±0.043 [6]   M☉
Radius 123±14 [6]   R☉
Luminosity 1,490±150 [5]   L☉
Surface gravity (log g)0.078±0.027 [6]   cgs
Temperature 3,500±250 [6]   K
Age 10 [6]   Gyr
Other designations
L2  Puppis, L02 Pup, HR  2748, CD−44°3227, HD  56096, LTT  2769, SAO  218549, HIP  34922
Database references
SIMBAD data
SPHERE and VLT NACO image of the nebulosity forming around L2 Puppis (Credit: ESO/P. Kervella) VLT SPHERE and NACO image of L2 Puppis.jpg
SPHERE and VLT NACO image of the nebulosity forming around L2 Puppis
(Credit: ESO/P. Kervella)

L2 Puppis (also known as HD 56096) is a giant star in the constellation of Puppis and is located between the bright stars Canopus and Sirius. It is a semi-regular pulsating star, and is intermittently visible to the naked eye.

Contents

History

The designation L2 has a tangled history. This star and another were both labelled with "L" by Nicolas-Louis de Lacaille when he created the constellation Puppis within Argo Navis. [7] The two stars were labelled as "1.L" and "2.L" by Johann Elert Bode in his star catalogue published in 1801. [8] Later authors used L1 and L2, usually with numeric subscripts (i.e. L1 and L2), [9] but occasionally as superscripts. [10] The subscripted designation is now universally used where typography allows for subscripts. [6] [11]

L2 Puppis was discovered to be variable by Benjamin Apthorp Gould in 1872, [12] and was listed in Uranometria Argentina as 73 G. Puppis with magnitude 5.10v. It has never been given a formal variable star designation, unlike L1 Puppis which is OU Puppis. [13]

Variability

A light curve for L2 Puppis, plotted from Hipparcos data L2PupLightCurve.png
A light curve for L2 Puppis, plotted from Hipparcos data

L2 Puppis varies in apparent magnitude by about two magnitudes with a period of 140 days. The average brightness also varies slowly over several years so that the total range is given as magnitude 2.6–6.0. Since 1995 the average brightness has dropped so that the 140-day variations are now between about magnitude 6 and 8. [4] [15] The variation in light may be caused by a combination of radial pulsations in the star's atmosphere and by dimming from circumstellar dust. [16]

Characteristics

L2 Puppis is most likely an red-giant branch star that has passed through the main sequence and is evolving to become a white dwarf. [5] It is shedding mass at the rate of about 5×10−7 M☉ per year, forming a circumstellar dust disk and bipolar plumes of gas that are thought to be the start of a "butterfly"-type planetary nebula. [6]

It has been calculated that the mass of L2 Puppis is currently about 0.66 M☉ and its original mass was close to one M☉ about 10 billion years ago. [6] Other calculations give higher masses, for example 2+1
−0.5 M☉, and younger ages such as 1.5 billion years. [11]

L2 Puppis has a visual 12th-magnitude companion. A hundred years ago, they were separated by about a minute of arc, but different proper motions mean that this is now about 1.5′ . [17]

Candidate planet

A candidate exoplanet has been found orbiting L2 Puppis every 4.69 years at a distance of 2.43  AU . The mass is highly uncertain, at 12 ± 16 MJ, and it might just be a dense clump of gas and dust. [6]

Related Research Articles

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Naos, also known by its Bayer designation of Zeta Puppis, is the brightest star in the constellation of Puppis.

<span class="mw-page-title-main">28 Andromedae</span> Star in the constellation Andromeda

28 Andromedae is a Delta Scuti variable star in the constellation Andromeda. 28 Andromedae is the Flamsteed designation. It also bears the variable star name GN Andromedae. Its apparent magnitude is 5.214, varying by less than 0.1 magnitudes.

<span class="mw-page-title-main">R Centauri</span> Variable star in the constellation Centaurus

R Centauri is a Mira variable star in the constellation Centaurus.

<span class="mw-page-title-main">NO Aurigae</span> Star in the constellation Auriga

NO Aurigae is a pulsating variable star in the constellation Auriga. It is an unusually-luminous asymptotic giant branch star about 3,500 light years away. It is a 6th magnitude star faintly visible to the naked eye under very good observing conditions.

<span class="mw-page-title-main">W Andromedae</span> Variable star in the constellation Andromeda

W Andromedae is a variable star in the constellation of Andromeda. It is classified as a Mira variable and S-type star, and varies from an apparent visual magnitude of 14.6 at minimum brightness to a magnitude of 6.7 at maximum brightness, with a period of approximately 397.3 days.

<span class="mw-page-title-main">HD 63032</span> Binary star system in the constellation Puppis

c Puppis, also known as HD 63032 and HR 3017, is a spectroscopic binary star in the constellation Puppis. Its apparent magnitude is of 3.61, making it the eight-brightest star in Puppis. The system is the brightest member of the open cluster NGC 2451, over two magnitudes brighter than every other star in the cluster. As the turnoff point of the cluster is currently around B7, the parameters of the system fit with cluster membership.

<span class="mw-page-title-main">HD 64440</span> Star in the constellation Puppis

HD 64440, also known as a Puppis, is a spectroscopic binary star in the constellation Puppis. Its apparent magnitude is 3.71. Located around 108 parsecs (350 ly) distant, the primary is a bright giant of spectral type K1.5II and the secondary is an early A-type star. They orbit with a period just under 7 years and eccentricity 0.38.

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HD 64760 is a class B0.5 supergiant star in the constellation Puppis. Its apparent magnitude is 4.24 and it is approximately 1,660 light years away based on parallax.

<span class="mw-page-title-main">QW Puppis</span> F3V star in the constellation Puppis

QW Puppis is a class F3V star in the constellation Puppis. Its apparent magnitude is 4.49 and it is approximately 69.5 light years away based on parallax.

<span class="mw-page-title-main">QZ Puppis</span> Star in the constellation Puppis

QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.

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MX Puppis is a class B1.5IV star in the constellation Puppis. Its apparent magnitude varies irregularly between magnitude 4.6 and 4.9 and it is classified as a Gamma Cassiopeiae variable. It is approximately 930 light years away based on parallax.

<span class="mw-page-title-main">HD 70555</span> Star in the constellation Puppis

HD 70555 is a class K2.5II-III star in the constellation Puppis. Its apparent magnitude is 4.83 and it is approximately 1,010 light years away based on parallax.

<span class="mw-page-title-main">OU Puppis</span> Star in the constellation Puppis

OU Puppis is a chemically peculiar class A0 star in the constellation Puppis. Its apparent magnitude is about 4.9 and it is approximately 188 light-years away based on parallax.

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<span class="mw-page-title-main">AC Herculis</span> Spectroscopic binary star in the constellation Hercules

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<span class="mw-page-title-main">S Cassiopeiae</span> Star in the constellation Cassiopeia

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<span class="mw-page-title-main">FU Tauri</span> Brown dwarf binary star system in the constellation Taurus

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<span class="mw-page-title-main">HD 152408</span> Star in the constellation of Scorpius

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References

  1. 1 2 3 4 5 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600.
  2. 1 2 3 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. 1 2 3 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  4. 1 2 Lykou, F.; Klotz, D.; Paladini, C.; Hron, J.; Zijlstra, A. A.; Kluska, J.; Norris, B. R. M.; Tuthill, P. G.; Ramstedt, S.; Lagadec, E.; Wittkowski, M.; Maercker, M.; Mayer, A. (2015). "Dissecting the AGB star L2 Puppis: A torus in the making". Astronomy & Astrophysics. 576: A46. arXiv: 1503.05031 . Bibcode:2015A&A...576A..46L. doi:10.1051/0004-6361/201322828. S2CID   11845036.
  5. 1 2 3 Uttenthaler, S. (2024-12-01). "The evolutionary state of the red giant star L2 Puppis". Astronomy & Astrophysics. 692: A224. doi:10.1051/0004-6361/202452173. ISSN   0004-6361.
  6. 1 2 3 4 5 6 7 8 9 10 Kervella, P.; Homan, W.; Richards, A. M. S.; Decin, L.; McDonald, I.; Montargès, M.; Ohnaka, K. (2016). "ALMA observations of the nearby AGB star L2 Puppis - I. Mass of the central star and detection of a candidate planet". Astronomy & Astrophysics. 596: A92. arXiv: 1611.06231 . Bibcode:2016A&A...596A..92K. doi:10.1051/0004-6361/201629877. S2CID   55298073.
  7. ↑ Coelum australe stelliferum ... H L Guerin & L F Delatour. 1763. p. 146.
  8. ↑ Johann Elert Bode (1801). Allgemeine Beschreibung und Nachweisung der Gestirne: Nebst Verzeichniss der geraden Aufsteigung und Abweichung von 17240 Sternen, Doppelsternen, Nebelflecken und Sternhaufen:(zu dessen Uranographie gehörig). Selbstverl. p. 76.
  9. ↑ Merrill, Paul Willard (1916). "Spectroscopic observations of stars of class MD". Publications of the Astronomical Observatory of the University of Michigan. 2: 48, 52. Bibcode:1916POMic...2...45M.
  10. ↑ Williams, A. Stanley (1897). "Observations of southern variables in 1885–86". Astronomical Journal. 18: 72. Bibcode:1897AJ.....18...71W. doi: 10.1086/102788 .
  11. 1 2 Chen, Zhuo; Nordhaus, Jason; Frank, Adam; Blackman, Eric G.; Balick, Bruce (2016). "Three-dimensional hydrodynamic simulations of L2 Puppis". Monthly Notices of the Royal Astronomical Society. 460 (4): 4182. arXiv: 1602.06142 . Bibcode:2016MNRAS.460.4182C. doi: 10.1093/mnras/stw1305 . S2CID   119195190.
  12. ↑ Innes, R. T. A.; Kapteyn, J. C. (1903). "Revision of the Cape Photographic Durchmusterung, Part II. Variable Stars, Miscellaneous Stars, etc". Annals of the Cape Observatory. 9: 18B, 48B. Bibcode:1903AnCap...9....2I.
  13. ↑ Benjamin Apthorp Gould (1879). Uranometria Argentina: Brightness and Position of Every Fixed Star, Down to the Seventh Magnitude, Within One Hundred Degrees of the South Pole. Paul Emile Coni. p. 171.
  14. ↑ "Light Curve". Hipparcos ESA. ESA. Retrieved 17 February 2022.
  15. ↑ Bedding, T. R.; Kiss, L. L.; Kjeldsen, H.; Brewer, B. J.; Dind, Z. E.; Kawaler, S. D.; Zijlstra, A. A. (2005). "The light curve of the semiregular variable L2 Puppis – II. Evidence for solar-like excitation of the oscillations". Monthly Notices of the Royal Astronomical Society. 361 (4): 1375–1381. arXiv: astro-ph/0507471 . Bibcode:2005MNRAS.361.1375B. doi: 10.1111/j.1365-2966.2005.09281.x . S2CID   16797010.
  16. ↑ Bedding, T. R.; Kiss, L. L.; Kjeldsen, H.; Brewer, B. J.; Dind, Z. E.; Kawaler, S. D.; Zijlstra, A. A. (August 2005). "The light curve of the semiregular variable L2 Puppis – II. Evidence for solar-like excitation of the oscillations". Monthly Notices of the Royal Astronomical Society . 361 (4): 1375–1381. arXiv: astro-ph/0507471 . Bibcode:2005MNRAS.361.1375B. doi: 10.1111/j.1365-2966.2005.09281.x . S2CID   16797010.
  17. ↑ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 .
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