NGC 1514

NGC 1514 is a planetary nebula in the zodiac constellation of Taurus,[2] positioned to the north of the star Psi Tauri along the constellation border with Perseus. Distance estimates for this nebula vary widely, with a range of 650–980 ly (200–300 pc) considered the most plausible.[3][4]

NGC 1514
Emission nebula
Planetary nebula
Observation data: J2000 epoch
Right ascension 04h 09m 16.98573s[1]
Declination+30° 46′ 33.4699″[1]
Distance~1,000 ly
Apparent magnitude (V)10.9[2]
Apparent dimensions (V)2′.2[2]
ConstellationTaurus

It was discovered by William Herschel on November 13, 1790, describing it as "a most singular phaenomenon" and forcing him to rethink his ideas on the construction of the heavens. Up until this point Herschel was convinced that all nebulae consisted of masses of stars too remote to resolve, but now here was a single star "surrounded with a faintly luminous atmosphere." He concluded: "Our judgement I may venture to say, will be, that the nebulosity about the star is not of a starry nature."[5][3]

This is a double-shell nebula that is described as, "a bright roundish amorphous PN" with a radius of around 65″ and a faint halo that has a radius of 90″.[6] It consists of an outer shell, an inner shell, and bright blobs.[7] An alternative description is of "lumpy nebula composed of numerous small bubbles" with a somewhat filamentary structure in the outer shell.[3] Infrared observations show a huge region of dust surrounds the planetary nebula, spanning 8.5 ly (2.6 pc). The combined mass of the gas and dust is estimated at 2.2±1.4 M☉[6]

The nebula originated from a binary star system with the designation HD 281679 from the Henry Draper Catalogue.[8] The bright, visible component is a giant star on the horizontal branch with a stellar classification of A0III, while the nebula-generating companion is now a hot, sub-luminous O-type star.[3] During the formation of the nebula, the pair shared a common envelope and had an orbital period of around 4–9 days. The progenitor star had a mass estimated at 4.5 times the mass of the Sun. When the progenitor entered its early-asymptotic giant branch phase and expanded to fill its roche lobe, mass transfer occurred and the pair spiraled inward by transferring their orbital energy into the expanding envelope.[7]

References
  1. 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.
  2. Finlay, Warren H. (2014), Concise Catalog of Deep-sky Objects, The Patrick Moore Practical Astronomy Series (2nd ed.), Springer Science & Business Media, p. 177, ISBN 978-3-319-03169-9.
  3. Ressler, Michael E.; et al. (December 2010), "The Discovery of Infrared Rings in the Planetary Nebula NGC 1514 During the WISE All-sky Survey", The Astronomical Journal, 140 (6): 1882–1890, arXiv:1011.3877, Bibcode:2010AJ....140.1882R, doi:10.1088/0004-6256/140/6/1882.
  4. Smith, H. (April 9, 2015), "On the distances of planetary nebulae", Monthly Notices of the Royal Astronomical Society, 449 (3): 2980–3005, arXiv:1409.3422, Bibcode:2015MNRAS.449.2980S, doi:10.1093/mnras/stv456.
  5. Herschel, William (February 10, 1791), "On Nebulous Stars, Properly So Called.", Philosophical Transactions of the Royal Society, 81: 71–88, Bibcode:1791RSPT...81...71H, doi:10.1098/rstl.1791.0006.
  6. Aryal, B.; et al. (February 2010), "A giant dusty bipolar structure around the planetary nebula NGC 1514", Monthly Notices of the Royal Astronomical Society, 402 (2): 1307–1312, Bibcode:2010MNRAS.402.1307A, doi:10.1111/j.1365-2966.2009.15966.x.
  7. Muthu, C.; Anandarao, B. G. (December 2003), "A Spatiokinematic Study of the Planetary Nebula NGC 1514", The Astronomical Journal, 126 (6): 2963–2970, Bibcode:2003AJ....126.2963M, doi:10.1086/379552.
  8. "NGC 1514". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-08-15.

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