532 Herculina
532 Herculina (herr'-kew-lye'-nə, English pronunciation: /ˈhɛrkjuˈlaɪnə/) is a very big asteroid, with a diameter of around 225 km.
| Discovery | |
|---|---|
| Discovered by | Max Wolf |
| Discovery date | April 20, 1904 |
| Designations | |
| 1904 NY | |
| Main belt | |
| Orbital characteristics | |
| Epoch 22 November 2003 (JD 2452600.5) | |
| Aphelion | 3.26 AU |
| Perihelion | 2.29 AU |
| 2.7719820 AU | |
| Eccentricity | 0.1777919 |
| 4.62 a | |
Average orbital speed | unknown |
| 142.15781° | |
| Inclination | 16.30843° |
| 107.65510° | |
| 76.86717° | |
| Physical characteristics | |
| Dimensions | 225 km |
| Mass | ~2.29×1019Kg [1] |
Mean density | ~4 g/cm³[1] |
| unknown | |
| unknown | |
| 9.404951 h | |
| Albedo | 0.16 |
| Temperature | unknown |
Spectral type | S |
| 8.82 to 11.99 | |
| 5.81 | |
| 0.228" to 0.073" | |
Discovery
changeIt was found on April 20th, 1904, by Max Wolf in Heidelberg, and initially catalogued as 1904 NY.[2] Where its name came from is not known; it may be named after the mythical Hercules, or after an unknown woman of that name. Most of the asteroids found by Wolf around this date were named for characters in operas, but if this name was also drawn from such a source, no explanation has been recorded.
Physical characteristics
changeHerculina is one of the twenty or so biggest members of the main asteroid belt.[3]
It has often been noted for its complex lightcurves, which made finding its shape and rotation somewhat hard. A set of 1982 speckle inferometry observations led to a simple preliminary model of Herculina as a three-axis object, perhaps 260 by 220 by 215 km. 1985 analysis of this data concluded there was a nonspherical shape with one bright spot, whilst a 1987 photometric astrometry study concluded the object was spherical with two dark spots (and rotated around a completely different pole), which was in turn negated by a 1988 thermal study which showed the object could not be spherical. By the late 1980s, the generally accepted model was a three-axis object with major albedo or topographical features.[4]
Recent (2002) modelling of photometric data shows that Herculina is not spherical, but a blocky shape not unlike a battered cuboid - or, as the analysis described it, it "resembles a toaster". This analysis indicates the presence of many big craters, similar to 253 Mathilde, but no major changes in albedo. The approximate ratios of the axes were suggested as 1:1.1:1.3, broadly consistent with earlier models if a bit more stretched.[5]
Moons
changeFollowing anomalous sightings during an occultation of the star SAO 1220774 in 1978, Herculina became the first asteroid to be "confirmed" to have an asteroid moon, with the parent asteroid estimated at a 216 km diameter and a moon of about 45 km orbiting at a distance of around 1,000 km.[6] However, careful studying in 1993, using the Hubble Space Telescope, could not locate a moon.[7]
References
change- ↑ 1.0 1.1 Masses and densities of minor planets Archived 2013-01-01 at the Wayback Machine - Yu. Chernetenko, O. Kochetova, and V. Shor
- ↑ Provisional elements of the minor planet 1904 NY. J. C. Hammond, Astronomical Journal, vol. 24, iss. 564, p. 105-105 (1904) ADS archive copy
- ↑ "20 Largest Asteroids". Archived from the original on 2004-12-05. Retrieved 2008-01-20.
- ↑ Speckle interferometry of asteroids (NASA CR-180438). J. Drummond, Steward Observatory, University of Arizona, May 31, 1988
- ↑ Models of Twenty Asteroids from Photometric Data Archived 2008-02-16 at the Wayback Machine. M. Kaasalainen, J. Torppa, and J. Piironen, Icarus 159, 369 – 395 (2002).
- ↑ Satellite of Minor Planet 532 Herculina Discovered During Occultation. David W. Dunham, The Minor Planet Bulletin, Volume 6, p.13-14 (December 1978) ADS archive copy
- ↑ Imaging observations of asteroids with Hubble Space Telescope Archived 2006-09-24 at the Wayback Machine. Storrs et al., Icarus 137, 260 – 268 (1999)
Other websites
change- Orbital simulation from JPL (Java) / Ephemeris