HM Sagittae

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HM Sagittae
HMSgeLightCurve.png
A light curve for HM Sagittae. The main plot shows 1-year averages of AAVSO visual band data. [1] The inset plot (adapted from Munari and Whitelock [2] ) shows near-infrared variability arising from the red giant's pulsations.
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Sagitta
Right ascension 19h 41m 57.080s [3]
Declination +16° 44′ 39.81″ [3]
Apparent magnitude  (V)10.99 [4]
Characteristics
Spectral type M7 [5]
Apparent magnitude  (pg)11.10 to 18 [6]
B−V color index 2.38 [4]
Variable type NC + M [6]
Astrometry
Proper motion (μ)RA: −0.443  mas/yr [3]
Dec.: −7.104  mas/yr [3]
Parallax (π)0.9735 ± 0.1033  mas [3]
Distance approx. 3,400  ly
(approx. 1,000  pc)
Details
Red giant
Radius 540 [7]   R☉
Luminosity 5,000 [8]   L☉
Temperature 3,000 [8]   K
White dwarf
Radius 0.08 [9]   R☉
Luminosity9,200 [9]   L☉
Temperature 200,000 [9]   K
Other designations
HM Sge, Nova Sge 1975, [10] SVS 2183 [11]
Database references
SIMBAD data

HM Sagittae is a dusty-type symbiotic nova in the northern constellation of Sagitta. [8] It was discovered by O. D. Dokuchaeva and colleagues in 1975 when it increased in brightness by six magnitudes (a factor of around 250 brighter). [12] The object displays an emission line spectrum similar to a planetary nebula and was detected in the radio band in 1977. [11] Unlike a classical nova, the optical brightness of this system did not rapidly decrease with time, although it showed some variation. It displays activity in every band of the electromagnetic spectrum from X-ray to radio. [13]

Observations in the infrared during 1978 showed this to be a very strong source with a spectrum that is consistent with a binary symbiotic system similar to V1016 Cyg. The cooler stellar component is emitting material that is then ionized by a hot component, with the emission spectrum coming from heated dust generated by the cooler star. [14] By 1983, the infrared emission of the system was shown to vary by a factor of 1.5 magnitudes in the K-band with a time scale of about 500 days. [15] High resolution spectral examination of the system in 1984 showed a bipolar outflow of matter with a velocity of 200 km/s. [13] A series of knots extend outward on both sides of the central star to an angular distance of 9 arcseconds. [16] The nebula surrounding the system shows a bipolar, S-shaped morphology, similar to R Aqr. [17]

The features of the system are consistent with a central red giant star being orbited by a compact object that is accreting matter from the giant. [13] The pair have an angular separation of 40±9  mas , with the axis aligned along a position angle of 130°±10°. Their physical separation is estimated at 50  astronomical units . [18] The giant component is most likely a Mira variable and measurements up to 1989 found a period of 527 days. [19] It is surrounded by a dusty shell that is mostly composed of silicates. [8] The compact object is a hot white dwarf with 70% of the mass of the Sun, [19] which is orbited by an accretion disk. The nova-like outburst of 1975 may have been generated by a burst of mass transfer from the giant to the white dwarf during the periastron passage of an eccentric orbit, leading to a thermonuclear outburst. [20]

Winds from both stars are colliding to produce a shock region that is a source of ultraviolet emission. [19] By 1985, a fading of the brightness and an increase in redness were observed, caused by dust obscuration. The hot component may be inhibiting dust formation around the giant except in the shadow region behind the star. This could explain observed individual dust obscuration events. [21]

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References

  1. ↑ "Download Data", aavso.org, AAVSO, retrieved 1 October 2021.
  2. ↑ Munari, U.; Whitelock, P. A. (March 1989), "Variable dust obscuration in the symbiotic Mira and very slow nova, HM Sge", Monthly Notices of the Royal Astronomical Society, 237: 45–50, Bibcode:1989MNRAS.237P..45M, doi: 10.1093/mnras/237.1.45P .
  3. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  4. 1 2 Høg, E.; et al. (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, ISBN   978-0333750889.
  5. ↑ Mürset, U.; Schmid, H. M. (1999), "Spectral classification of the cool giants in symbiotic systems", Astronomy and Astrophysics Supplement, 137 (3): 473, Bibcode:1999A&AS..137..473M, doi: 10.1051/aas:1999105 .
  6. 1 2 Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports , 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  7. ↑ Taranova, O. G.; Shenavrin, V. I. (2000), "Infrared Photometry of the Symbiotic Novae V1016 Cyg and HM Sge in 1978-1999", Astronomy Letters, 26 (9): 600, Bibcode:2000AstL...26..600T, doi:10.1134/1.1307894, S2CID   120096176.
  8. 1 2 3 4 Sacuto, S.; Chesneau, O. (January 2009), "On the morphology of the compact dust shell in the symbiotic system HM Sagittae", Astronomy and Astrophysics, 493 (3): 1043–1048, arXiv: 0812.1896 , Bibcode:2009A&A...493.1043S, doi:10.1051/0004-6361:200810934, S2CID   14886524.
  9. 1 2 3 Schild, H.; Eyres, S. P. S.; Salama, A.; Evans, A. (2001), "ISO observations of symbiotic stars. I. HM Sge", Astronomy and Astrophysics, 378: 146, Bibcode:2001A&A...378..146S, doi: 10.1051/0004-6361:20011155 .
  10. ↑ "HM Sge", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2022-02-09.
  11. 1 2 Feldman, P. A. (October 1977), "The Detection of Radio Emission from the New Optical Emission Variable HM Sagittae", Journal of the Royal Astronomical Society of Canada, 71: 386, Bibcode:1977JRASC..71..386F.
  12. ↑ Dokuchaeva, O. D. (October 1976), "A New Emission Object", Information Bulletin on Variable Stars, 1189: 1, Bibcode:1976IBVS.1189....1D.
  13. 1 2 3 Solf, J. (October 1984), "High-resolution observations of bipolar mass flow from the symbiotic star HM Sagittae", Astronomy and Astrophysics, 139: 296–304, Bibcode:1984A&A...139..296S.
  14. ↑ Puetter, R. C.; et al. (July 1978), "Infrared spectra of HM Sagittae and V1016 Cygni", Astrophysical Journal, 223: L93–L95, Bibcode:1978ApJ...223L..93P, doi: 10.1086/182736 .
  15. ↑ Taranova, O. G.; Iudin, B. F. (January 1983), "V1016 Cygni and HM Sagittae : binary stellar systems", Astronomy and Astrophysics, 117: 209–214, Bibcode:1983A&A...117..209T.
  16. ↑ Corradi, R. L. M.; et al. (August 1999), "The optical nebulae around the symbiotic Miras He 2-147, HM Sagittae and V1016 Cygni", Astronomy and Astrophysics, 348: 978–989, Bibcode:1999A&A...348..978C.
  17. ↑ Hack, Warren J.; Paresce, Francesco (November 1993), "Imaging the Bipolar Nebula around HM Sagittae", Publications of the Astronomical Society of the Pacific, 105: 1273, Bibcode:1993PASP..105.1273H, doi: 10.1086/133307 , S2CID   121305970.
  18. ↑ Eyres, S. P. S.; et al. (April 2001), "The Inner Nebula and Central Binary of the Symbiotic Star HM Sagittae", The Astrophysical Journal, 551 (1): 512–519, arXiv: astro-ph/0101189 , Bibcode:2001ApJ...551..512E, doi:10.1086/320086, S2CID   119332145.
  19. 1 2 3 Sanad, M. R.; Abdel-Sabour, M. A. (April 2020), "Spectral Behavior of the Symbiotic Nova HM Sge in the Ultraviolet", Revista Mexicana de Astronomía y Astrofísica, 56: 63–69, Bibcode:2020RMxAA..56...63S, doi: 10.22201/ia.01851101p.2020.56.01.08 .
  20. ↑ Chochol, D.; et al. (February 2004), "Long-term photometry of the symbiotic nova HM Sge", Contributions of the Astronomical Observatory Skalnaté Pleso, 34 (1): 5–19, Bibcode:2004CoSka..34....5C.
  21. ↑ Munari, U.; Whitelock, P. A. (March 1989), "Variable dust obscuration in the symbiotic Mira and very slow nova, HM Sge.", Monthly Notices of the Royal Astronomical Society, 237: 45P–50P, Bibcode:1989MNRAS.237P..45M, doi: 10.1093/mnras/237.1.45P .

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