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LoTr 1

LoTr 1
Emission nebula
Planetary nebula
Observation data: J2000 epoch
Right ascension05h 55m 06.6s[1]
Declination−22° 54′ 02″[1]
Distance5,875[2] ly
Apparent diameter2' 26" ± 4"[3]
ConstellationLepus
DesignationsPN DeHt 1, PK 228-22 1, PN G228.2-22.1, V* AB Lep[1]
See also: Lists of nebulae

LoTr 1 (Longmore-Tritton 1) is a bubble-shaped elliptical nebula with a binary central star system. LoTr 1 was discovered with 11 other planetary nebula under the LoTr Catalog and was discovered in 1980 by astronomers A.J Longmore and S.B. Tritton using the UK Schmidt Telescope.[4]

Characteristics

The nucleus of LoTr 1 has similar properties that can be found in other planetary nebulae like Abell 35 and LoTr 5, where the central star in nucleus consist of giant star and hot companion detected by International Ultraviolet Explorer.[5] The nebula features a central inner shell with an angular diameter of 47 ± 4" and a expansion age of ~17,000 yr. And features an outer shell with a more irregular shape that has a diameter of 4 ± 26" and an expansion age of ~35,000 yr.[3] The inner shell has an expansion velocity of ~25 ± 4 km while the outer shell is estimated to be ~25 ± 4 km.[6] The nebula is significantly brighter in ionized oxygen [O III] wavelengths compared to other emissions. The two slightly elongated shells possess different spatial orientations, indicating separate historical mass-transfer or ejection episodes from the binary interaction.[3] The double-peaked Hα mission lines remain a mystery, but have been hypothesized to come from the active accretion disk.

AB Leporis

AB Leporis is a binary star system that contains a variable K-type subgiant star with emission line and a hot white dwarf companion.[3] The K-type giant star is found to have barium abundance of 0.5 or greater thus classifies it as a Barium star. The K-type giant features a rapid rotation period of 6.4 days, which proves past mass accretion activity.[3] The star has a orbital period of ~100 and ~1,500 years. The KII giant was spun up to a rapid 6.4-day rotation via wind accretion. This occurred when the primary star was in the Asymptotic giant branch (AGB). The star system has an orbital period of ~11.28 yr.[7] The radial velocity of the binary is ~7.4 yr. The lack of observed [Fe V] lines and the absence of the [C III] multiplet imposes a temperature limit of ~105,000 K.[8] The radius for the giant star is ~9.7R while the hot White dwarf has a radius of 0.44R, indicating that it is about to enter white dwarf cooling sequence.[9]

References

  1. ^ a b c "V* AB Lep". simbad.cds.unistra.fr.
  2. ^ "Longmore Tritton 1 PN in Lepus". chart32.de.
  3. ^ a b c d e Tyndall, A. A.; Jones, D.; Boffin, H. M. J.; Miszalski, B.; Faedi, F.; Lloyd, M.; Boumis, P.; López, J. A.; Martell, S.; Pollacco, D.; Santander-García, M. (2013-12-11). "Two rings but no fellowship: LoTr 1 and its relation to planetary nebulae possessing barium central stars". Monthly Notices of the Royal Astronomical Society. 436 (3): 2082–2095. doi:10.1093/mnras/stt1713. ISSN 1365-2966.
  4. ^ Longmore, A. J.; Tritton, S. B. (1980). "A second list of new planetary nebulae found on United Kingdom 1.2-m Schmidt telescope plates". Monthly Notices of the Royal Astronomical Society. 193 (3): 521–524. doi:10.1093/mnras/193.3.521. ISSN 0035-8711.
  5. ^ Bond, Howard E.; Ciardullo, Robin; Meakes, Michael G. (1993). "The Abell 35-Type Planetary Nuclei". Symposium - International Astronomical Union. 155: 397. doi:10.1017/S0074180900171864. ISSN 0074-1809.
  6. ^ Weinberger, R. (May 1989). "A catalogue of expansion velocities of galactic planetary nebulae". Astronomy & Astrophysics. 78 (301–324): 301. Bibcode:1989A&AS...78..301W.
  7. ^ Martínez, C. I.; Mauas, P. J. D.; Buccino, A. P. (2022-05-14). "Activity cycles in RS CVn-type stars". Monthly Notices of the Royal Astronomical Society. 512 (4): 4835–4845. arXiv:2111.05911. Bibcode:2022MNRAS.512.4835M. doi:10.1093/mnras/stac755.
  8. ^ Werner, K.; Reindl, N.; Löbling, L.; Pelisoli, I.; Schaffenroth, V.; Rebassa-Mansergas, A.; Irawatuli, P.; Ren, J. (October 2020). "An extremely hot white dwarf with a rapidly rotating K-type subgiant companion: UCAC2 46706450". Astronomy & Astrophysics. 642: 13. arXiv:2009.02968. Bibcode:2020A&A...642A.228W. doi:10.1051/0004-6361/202038574. A288.
  9. ^ Bhattacharjee, S.; Reindl, N.; Bond, H. E.; Werner, K.; Zeimann, G. R.; Jones, D.; El-Badry, K.; Mackensen, N.; Chornay, N.; Kulkarni, S. R.; Caiazzo, I.; Roestel, J. V.; Rodriguez, A. C.; Prince, T. A.; Laher, R. R.; Rusholme, B.; Smith, R. (17 October 2025). "Variability of Central Stars of Planetary Nebulae with the Zwicky Transient Facility. II. Long-timescale Variables including Wide Binary and Late Thermal Pulse Candidates". Astronomical Society of the Pacific. 137 (10): 10. arXiv:2502.18651. Bibcode:2025PASP..137j4206B. doi:10.1088/1538-3873/ae051e.

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