|Discovered by||John Russell Hind|
|Discovery date||August 13, 1847|
|MPC designation||(7) Iris|
|Epoch 27 April 2019 (JD 2458600.5)|
|Aphelion||2.937 AU (439.4 Gm)|
|Perihelion||1.834 AU (274.4 Gm)|
|2.385 AU (356.8 Gm)|
|3.68 a (1345.375 d)|
Average orbital speed
|Proper orbital elements|
Proper semi-major axis
Proper mean motion
|97.653672 deg / yr|
Proper orbital period
Precession of perihelion
|38.403324 arcsec / yr|
Precession of the ascending node
|−46.447128 arcsec / yr|
|Dimensions||268 km × 234 km × 180 km|
± (5 km × 4 km × 6 km)
225 km × 190 km × 190 km
199.8±10 km (IRAS)
Equatorial surface gravity
Equatorial escape velocity
|7.138843 h (0.2974518 d)|
Equatorial rotation velocity
max: 275 K (+2°C)
|6.7 to 11.4|
|0.32" to 0.07"|
Iris (minor planet designation: 7 Iris) is a large main-belt asteroid orbiting the Sun between Mars and Jupiter. It is the fourth-brightest object in the asteroid belt. It is classified as an S-type asteroid, meaning that it has a stony composition.
Discovery and name
Iris was named after the rainbow goddess Iris in Greek mythology, who was a messenger to the gods, especially Hera. Her quality of attendant of Hera was particularly appropriate to the circumstances of discovery, as Iris was spotted following 3 Juno by less than an hour of right ascension (Juno is the Roman equivalent of Hera).
Iris is an S-type asteroid. Its surface likely exhibits albedo differences, with possibly a large bright area in the northern hemisphere. Overall the surface is very bright and is probably a mixture nickel-iron metals and magnesium- and iron-silicates. Its spectrum is similar to that of L and LL chondrites with corrections for space weathering, so it may be an important contributor of these meteorites. Planetary dynamics also indicates that it should be a significant source of meteorites.
Iris's bright surface and small distance from the Sun make it the fourth-brightest object in the asteroid belt after Vesta, Ceres, and Pallas. It has a mean opposition magnitude of +7.8, comparable to that of Neptune, and can easily be seen with binoculars at most oppositions. At typical oppositions it marginally outshines the larger though darker Pallas. But at rare oppositions near perihelion Iris can reach a magnitude of +6.7 (last time on October 31, 2017 reaching a magnitude of +6.9), which is as bright as Ceres ever gets.
A study by Hanus et al. using data from the VLT's SPHERE instrument names eight craters, and seven recurring features who remain nameless due to a lack of consistency and their occurrence on the edge of Iris. The tentative naming scheme is that of colors in Latin. It is unknown whether these names are accepted by the IAU. All 8 features are craters, the remaining 7 features are unknown, and are named A through G.
Lightcurve analysis indicates a somewhat angular shape and that Iris's pole points towards the ecliptic coordinates (β, λ) = (10°, 20°) with a 10° uncertainty. This gives an axial tilt of 85°, so that on almost a whole hemisphere of Iris, the sun does not set during summer, and does not rise during winter. On an airless body this gives rise to very large temperature differences.
- Calculated based on parameters calculated by J. Hanuš et al.
- Hanuš, J.; Marsset, M.; Vernazza, P.; Viikinkoski, M.; Drouard, A.; Brož, M.; et al. (24 April 2019). "The shape of (7) Iris as evidence of an ancient large impact?". Astronomy & Astrophysics. 624 (A121). arXiv:1902.09242. Bibcode:2018DPS....5040406H. doi:10.1051/0004-6361/201834541.
- Oxford English Dictionary
- "JPL Small-Body Database Browser: 7 Iris" (2018-03-27 last obs.). Jet Propulsion Laboratory. Retrieved 17 June 2019.
- "AstDyS-2 Iris Synthetic Proper Orbital Elements". Department of Mathematics, University of Pisa, Italy. Retrieved 1 October 2011.
- Kaasalainen, M.; et al. (2002). "Models of twenty asteroids from photometric data" (PDF). Icarus. 159 (2): 369. Bibcode:2002Icar..159..369K. doi:10.1006/icar.2002.6907.
- Donald H. Menzel & Jay M. Pasachoff (1983). A Field Guide to the Stars and Planets (2nd ed.). Boston, MA: Houghton Mifflin. p. 391. ISBN 0-395-34835-8.
- "Bright Minor Planets 2006". Minor Planet Center. Retrieved 21 May 2008.[permanent dead link]
- Hoffmann, M.; E. H. Geyer (1993). "Spots on 4-VESTA and 7-IRIS - Large Areas or Little Patches". Astronomy and Astrophysics Supplement. 101: 621. Bibcode:1993A&AS..101..621H.
- Y. Ueda et al. Surface Material Analysis of the S-type Asteroids: Removing the Space Weathering Effect from Reflectance Spectrum, 34th Annual Lunar and Planetary Science Conference, March 17–21, 2003, League City, Texas, abstract no.2078 (2003).
- Migliorini, F.; et al. (1997). "(7) Iris: a possible source of ordinary chondrites?". Astronomy & Astrophysics. 321: 652. Bibcode:1997A&A...321..652M.
- Odeh, Moh'd. "The Brightest Asteroids". Jordanian Astronomical Society. Archived from the original on 13 August 2007. Retrieved 16 July 2007.
- Vernazza, Pierre. "ESO/VLT/SPHERE Survey of D>100km Asteroids : First Results" (PDF). Lunar and Planetary Institute. USRA. Retrieved 16 September 2019.
- Shape model deduced from lightcurve (M. Kaasalainen 2002)
- 2011-Feb-19 Occultation (Durech Model) / (2011 Asteroidal Occultation Results for North America)
- "Discovery of Iris", MNRAS 7 (1847) 299
- JPL Ephemeris
- "Elements and Ephemeris for (7) Iris". Minor Planet Center. Archived from the original on 4 March 2016. (displays Elong from Sun and V mag for 2011)
- 7 Iris at AstDyS-2, Asteroids—Dynamic Site
- 7 Iris at the JPL Small-Body Database