Minkowski 4-18 (M 4-18) is a planetary nebula or protoplanetary nebula[6] in the deep northern constellation of Camelopardalis. Distance estimates range widely across publications between 1–7 kpc,[7] though a 2022 paper gives a distance of 5,230 parsecs (17,100 light-years).[2] The nebula appears to be very young,[8] at about 3,100 years old.[7] Notably, the central star of the nebula is a very cool, late-type Wolf-Rayet star of spectral type [WC11].[2]
This object was discovered by German-American astronomer Rudolph Minkowski in 1959.[11] The nebula extends about 0.06 parsecs (0.20 light-years) from its center.[5] As early as 1974, the central star was known to be among the coolest carbon-sequence (type WC) Wolf-Rayet stars.[12] The nebula has a mass of 0.08 M☉[7] and an electron temperature, that is the average kinetic energy of electrons within the plasma, of 8,160 K (7,890 °C; 14,230 °F).[13]
The central star has only 62% the mass of the Sun but is 2.4 times as large. It radiates 5,250 times the luminosity of the Sun from its photosphere at an effective temperature of 31,000 K (30,700 °C; 55,300 °F), according to De Marco & Crowther (1999).[7] Some other sources, such as Acker et al. (2002), find a lower temperature of around 25,000 K.[5]
Variability
The center star of M 4-18, together with two other objects M 2-54 and NGC 2392, was reported to be a low-amplitude variable in 1996, brightening by 0.03 mag over a 7-hour observation period in the night of 12 December 1995.[14]
Reddening
The star is reddened substantially[11] at EB−V = 0.75±0.10.[13] The reddening in the ultraviolet region is considered anomalous, as different methods yield very different results for EB−V. This is possibly caused by an undetected shell of circumstellar dust.[8] The infrared reddening profile can be explained by grains of amorphous carbon of a uniform size.[6]
Spectra and abundances
The central star displays broad emission lines of C+, C2+, and C3+ (C II, C III, and C IV in spectroscopic notation),[15] of which the lines of C+ are the strongest, consistent with the star's carbon-rich, Wolf-Rayet nature and relatively low effective temperature.[13] The carbon lines overlay the nebula's emission lines, namely neutral hydrogen (H I), as well as the forbidden lines, indicated by the square brackets, of singly ionized nitrogen ([N II]) and sulfur ([S II]). The forbidden line [O III] (O2+; wavelength 4959–5007 Å) is unusually weak, similar to HD 184738 (Campbell's Hydrogen Star).[15] Compared to HD 184738, M 4-18 shows weaker lines of C IV, O IV (O3+), and N V (N4+), implying that atoms in this nebula are in a less excited state.[16]
A 1980 paper claimed that the nebula was deficient in nitrogen and oxygen,[16] but a study in 1995 found a solar-like abundance of carbon, nitrogen, and neon, as well as an oxygen content twice as high as that of the Sun. In contrast, it is very poor in sulfur, only containing 10% as much as the Sun.[6] The reported enrichment in oxygen is dubious, however, as a paper published in 2022 presented a slightly subsolar oxygen abundance. The same paper described an overabundance of xenon.[2]
Weak P Cygni emission features were confirmed in 1984, evidence of stellar winds radiating away from the central star reaching a velocity of approximately 300 km/s.[17]
^ abCutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
^ abLeuenhagen, U.; Hamann, W. R.; Jeffery, C. S. (1996). "Spectral analyses of late-type WC central stars of planetary nebulae". Astronomy & Astrophysics. 312: 167–185. Bibcode:1996A&A...312..167L.
^ abSabbadin, F. (April 1980). "Spectroscopic observations of the compact PN M 4-18". Astronomy & Astrophysics. 84: 216–219. Bibcode:1980A&A....84..216S.
^Shaw, R. A. (September 1984). "The Wind from the Nucleus of the Planetary Nebula M4-18". Bulletin of the American Astronomical Society. 16: 975. Bibcode:1984BAAS...16Q.975S.
^Szczerba, R.; Volk, K.; Górny, S. K. (2003). Sun Kwok; Michael Dopita; Ralph Sutherland (eds.). "ISO-SWS spectra of [WR] planetary nebulae". Planetary Nebulae: Their Evolution and Role in the Universe, Proceedings of the 209th Symposium of the International Astronomical Union. 209. Canberra, Australia: Astronomical Society of the Pacific: 301. Bibcode:2003IAUS..209..301S.
