Draft:Jonckheere 900
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Comment: Good start but unfortunately i can't find any mention of the Planetary nebula in your mentioned astronomy journal. Also please try to improve your grammar skills Abdullah1099 (talk) 12:04, 10 August 2026 (UTC)
| Emission nebula | |
|---|---|
| Planetary nebula | |
 Image taken by the Hubble Space Telescope[1] | |
| Observation data: J2000 epoch | |
| Right ascension | 6h 25m 57.237s[2] |
| Declination | +17° 47′ 27.53″[2] |
| Distance | 12,687-19,569 ly |
| Constellation | Gemini[1] |
| Designations | PK 194+02 1, PN G194.2+02.5, VV 28, ARO 92[2] |
Jonckheere 900 (J900) is a Bipolar planetary nebula discovered in 1912 by French astronomer R. Jonckheere using the Lille University Observatory. Although he initially thought it was a double star, The Hubble Space Telescope later determined the object was not a double star.[3][1]
J900 has a distance (D) ranging from 3.89 kpc to 6 kpc with an average value of ~4.6 kpc,[4][5][6] which predicts that the ionization front is located at ~8.5 arcseconds away from the central star. The nebula has a temperature floor of ~829 K, which is derived from an H2 temperature of 755±36 K.[7]
The J900 nebula was detected to have [Kr III] and [Se IV] lines.[8] Forbidden Lines of Kr, Rb, and Xe were detected in the BOES spectrum while the F line was detected using the mid-IR Spitzer Infrared Spectrograph.[9] The nebula features H2 lines emitted from both a ~670 K warm and a ~3200 K hot reigon. Emission lines with calculated Te and ne include: the [O III] line with Te = 11,600±1160 K and ne = 3600±1160 cm-3,[10] the [S III] line with Te = 13,000 K, the [N II] line with Te = 11,500 K, the [O II] line with Te = 10,300 K and ne = 3980 cm-3, the [S II] line with Te = 7800 K and ne = 3600 cm-3, and the [Ar IV] line with ne = 8240 cm-3.[11]
A unnamed faint field star located roughly 11 arcseconds away from the central star is right next to J900, giving the illusion of a double system.
Central star
[edit]The star has an effective temperature of ~134,800 K calculated using the observed I(He II 4686 Å)/I(H β) ratio.[12] The star evolved from an initial mass of ~2.0 M⊙.[13] The central star has a visual magnitude of 17.8 mag.
References
[edit]- 1 2 3 "Hubble Sees J 900 Masquerading as a Double Star". NASA Science (.gov). ESA/Hubble and NASA. Retrieved 28 March 2013.
- 1 2 3 "PN VV 28". simbad.cds.unistra.fr.
- ↑ Bernard, E. E. (September 1917). "THE OBJECT R. JONCKHEERE 900,". The Astronomical Journal. 719. Albany, N.Y. , U.S.A.: Dudley Observatory: 208. Bibcode:1917AJ.....30..208B.
- ↑ Stanghellini, L.; Haywood, M. (July 2018). "Galactic Planetary Nebulae as Probes of Radial Metallicity Gradients and Other Abundance Patterns". The Astrophysical Journal. 862 (1): 11. arXiv:1806.02276. Bibcode:2018ApJ...862...45S. doi:10.3847/1538-4357/aacaf8. 45.
- ↑ Kingsburgh, R. L.; Barlow, M. J. (July 1992). "Distances for galactic planetary nebulae using mean [O II] doublet ratio electron densities". Monthly Notices of the Royal Astronomical Society. 257: 317–339. Bibcode:1992MNRAS.257..317K. doi:10.1093/mnras/257.2.317.
- ↑ Stanghellini, L.; Shaw, R. A.; Villaver, E. (2008). "The Magellanic Cloud Calibration of the Galactic Planetary Nebula Distance Scale". The Astrophysical Journal. 689 (1): 194–202. arXiv:0807.1129. Bibcode:2008ApJ...689..194S. doi:10.1086/592395.
- ↑ Hora, J. H.; Latter, W. B.; Deutsch, L. K. (1999). "Investigating the Near-Infrared Properties of Planetary Nebulae. II. Medium-Resolution Spectra". The Astrophysical Journal Supplement Series. 124 (1): 195. arXiv:astro-ph/9904202. Bibcode:1999ApJS..124..195H. doi:10.1086/313256.
- ↑ Sterling, N. C.; Dinerstein, H. L.; Hwang, S. (September 2009). "Improved Neutron-Capture Element Abundances in Planetary Nebulae". Publications of the Astronomical Society of Australia. 26 (3): 339–344. arXiv:0812.2221. Bibcode:2009PASA...26..339S. doi:10.1071/AS08067.
- ↑ Houck, J. R.; Roellig, T. L.; van Cleve, J.; Forrest, W. J.; Herter, T.; Lawrence, C. R.; Matthews, K.; Reitsema, H. J.; Soifer, B. T.; Watson, D. M. (2004). "The Infrared Spectrograph (IRS) on the Spitzer Space Telescope". The Astrophysical Journal Supplement Series. 154 (1): 18–24. arXiv:astro-ph/0406167. Bibcode:2004ApJS..154...18H. doi:10.1086/423134.
- ↑ Sterling, N. C.; Dinerstein, H. L. (2008). "The Abundances of Light Neutron-Capture Elements in Planetary Nebulae. II. s-Process Enrichments and Interpretation". The Astrophysical Journal Supplement Series. 174 (1): 158. Bibcode:2008ApJS..174..158S. doi:10.1086/520845.
- ↑ Kingsburgh, R. L.; Barlow, M. J. (November 1994). "Elemental abundances for a sample of southern galactic planetary nebulae". Monthly Notices of the Royal Astronomical Society. 271 (2): 257–299. Bibcode:1994MNRAS.271..257K. doi:10.1093/mnras/271.2.257.
- ↑ Dopita, M. A.; Meatheringham, S. J. (August 1991). "Photoionization Modeling of Magellanic Cloud Planetary Nebulae. II". The Astrophysical Journal. 377: 480. Bibcode:1991ApJ...377..480D. doi:10.1086/170377.
- ↑ Karakas, A. I.; Carlos, M.; Lugaro, M.; Cseh, B.; Kamath, D.; García-Hernández, D. A. (June 2018). "Heavy-element yields and abundances of asymptotic giant branch models with a Small Magellanic Cloud metallicity". Monthly Notices of the Royal Astronomical Society. 477 (1): 421–437. arXiv:1803.02028. Bibcode:2018MNRAS.477..421K. doi:10.1093/mnras/sty625.