|Observation data: J2000 epoch|
|Right ascension||07h 42m 16.83s |
|Declination||−14° 42′ 52.1″|
|Distance||4,200 ly (1,300 pc)|
|Apparent magnitude (V)||9.47|
|Apparent dimensions (V)||1′|
|Absolute magnitude (V)||-1.4[b]|
|Designations||OH 231.84 +4.22,
Rotten Eggs Nebula
The Calabash Nebula, also known as the Rotten Egg Nebula or by its technical name OH 231.84 +4.22, is a protoplanetary nebula (PPN) 1.4 light years (13 Pm) long and located some 5,000 light years (47 Em) from Earth in the constellation Puppis. The name "Calabash Nebula" was first proposed in 1989 in an early paper on the expected nebular dynamics, based on the nebula's appearance  The Calabash is an almost certain member of the open cluster Messier 46, as it has the same distance, radial velocity, and proper motion.
The object is sometimes called the Rotten Egg Nebula because it contains a relatively large amount of sulfur. The densest parts of the nebula are composed of material ejected recently by the central star and accelerated in opposite directions. This material, shown as yellow in the image, is zooming away at speeds up to one and a half million kilometers per hour (one million miles per hour). Most of the star's original mass is now contained in these bipolar gas structures.
A team of Spanish and US astronomers used NASA's Hubble Space Telescope to study how the gas stream rams into the surrounding material, shown in blue. They believe that such interactions dominate the formation process in planetary nebulae. Due to the high speed of the gas, shock-fronts are formed on impact and heat the surrounding gases. Although computer calculations had predicted the existence and structure of such shocks for some time, previous observations had not been able to prove the theory.
This new Hubble image used filters that only let through light from ionized hydrogen and nitrogen atoms. Astronomers were able to distinguish the warmest parts of the gas heated by the violent shocks and found that they form a complex double-bubble shape. The bright yellow-orange colors in the picture show how dense, high-speed gas is flowing from the star, like supersonic speeding bullets ripping through a medium in opposite directions. The central star itself is hidden in the dusty band at the center.
Much of the gas flow observed today seems to stem from a sudden acceleration that took place only about 800 years ago. The astronomers believe that 1,000 years from now, the Calabash Nebula will become a fully developed planetary nebula, like a butterfly emerging from its chrysalis.
In wide field images the Calabash nebula is visible near the bright planetary nebula NGC 2438 in deep photographs. Although the Calabash nebula is at the same distance as M46, NGC 2438 is a larger object in the background. The Calabash nebula is shown in this broadband image to the lower right.
- (SIMBAD 2007)
- (Kastner et al. 1998)
- Vickers S.B.; Frew D.J.; Parker Q.A.; Bojicic I.S. (2015). "New light on Galactic post-asymptotic giant branch stars - I. First distance catalogue". Monthly Notices of the Royal Astronomical Society 447: 1673. arXiv:1403.7230. Bibcode:2015MNRAS.447.1673V. doi:10.1093/mnras/stu2383.
- Icke, Vincent; Preston, Heather L. (1989), "The Dynamics of the Calabash Nebula", Astronomy and Astrophysics (NASA Astrophysics Data System (ADS)) 211 (2): 409–412, Bibcode:1989A&A...211..409I
- Kastner, Joel H.; Weintraub, David A.; Merrill, K. M.; Gatley, Ian (1998), "Direct Detection of the Mira at the Heart of OH 231.8+4.2", The Astronomical Journal (SIMBAD, Centre de Données Astronomiques de Strasbourg) 116 (3): 1412–1418, Bibcode:1998AJ....116.1412K, doi:10.1086/300520
- SInMBAD (January 4, 2007), Results for Red Rectangle, SIMBAD, Centre de Données Astronomiques de Strasbourg
|Wikimedia Commons has media related to Calabash Nebula.|
- PIA04228: Rotten Egg Nebula, NASA Planetary Photojournal
- The Rotten Egg Planetary Nebula, APOD 1999 November 1
- The Making of the Rotten Egg Nebula, APOD 2001 September 3
- Calabash Nebula at Constellation Guide
- Calabash Nebula imaged and interpreted by Bo Reipurth at the European Southern Observatory in 1987