22 Kalliope

22 Kalliope
	Kalliope and satelliteLinusas seen by theW.M. Keck II telescopein 2010
Discovery
Discovered by	John Russell Hind
Discovery date	16 November 1852
Designations
MPC designation	(22) Kalliope
Pronunciation	/kəˈlaɪ.əpi/kə-LY-ə-pee
Named after	ΚαλλιόπηKalliopē
Minor planet category	Main belt
Adjectives	Kalliopean/kəˌlaɪ.əˈpiːən/kə-LY-ə-PEE-ən
Orbital characteristics
	Epoch23 July 2010 (JD2455400.5)
Aphelion	479.98Gm(3.2085AU)
Perihelion	391.03 Gm (2.6139 AU)
Semi-major axis	435.09 Gm (2.9112 AU)
Eccentricity	0.10213
Orbital period (sidereal)	1814.3 d (4.97yr)
Mean anomaly	282.54°
Inclination	13.703°
Longitude of ascending node	66.17°
Argument of perihelion	355.03°
Knownsatellites	Linus
Physical characteristics
Dimensions	235 km × 144 km × 124 km; 190 km × 125 km
Mean diameter	150±5 km; 166.2±2.8 km; 167.536±3.053 km; 181.0±4.6 km(IRAS);
Flattening	0.41
Mass	(7.7±0.4)×1018kg; (8.16±0.26)×1018kg; 7.36×1018kg; (6.30±0.50)×1018kg
Meandensity	4.36±0.50 g/cm3; 3.35±0.33 g/cm3; 2.37±0.40 g/cm3; 2.03±0.16 g/cm3;
Synodic rotation period	0.17285 days (4.1483 h)
Geometric albedo	0.198; 0.17; 0.166 ± 0.005
Spectral type	M(Tholen); X(SMASS); X(Bus-DeMeo) ;
Absolute magnitude(H)	6.81

22 Kalliope(/kəˈlaɪ.əpi/;kə-LY-ə-pee) is a largeM-type asteroidfrom theasteroid beltdiscovered byJ. R. Hindon 16 November 1852. It is named afterCalliope,theGreek Museofepic poetry.It is orbited by a small moon namedLinus.

Characteristics

Kalliope is somewhat elongated, approximately 166 km indiameter,^[3]and slightly asymmetric, as evidenced by resolved images taken with theVLTat theEuropean Southern Observatory.This new diameter, which was measured by observing mutual eclipses of Kalliope and Linus, is 8% smaller than that calculated fromIRASobservations.^[3]

The spectrum of Kalliope is anM-type,indicating that its surface may be partially composed ofiron–nickelmetal. The asteroid's density is about 3.4 g/cm³.^[3]Since the asteroid is likely to be arubble pile,accounting for a possible porosity of 20–40% leads to the material density of 4.2–5.8 g/cm³,which means that Kalliope is probably made of a mixture of metal withsilicates.^[3]Spectroscopic studies have shown, however, evidence ofhydratedminerals^[9]and silicates,^[10]which indicate rather a stony surface composition. Kalliope also has a low radar albedo,^[6]which is inconsistent with a purely metallic surface.

Lightcurve analysis indicates that Kalliope's pole most likely points towardsecliptic coordinates(β, λ) = (−23°, 20°) with a 10° uncertainty,^[11]^[7]which gives Kalliope anaxial tiltof 103°. Kalliope's rotation is then slightly retrograde.

Between 2004 and 2021, 22 Kalliope has been observed tooccultfifteen stars.

Satellite

Kalliope has one known natural satellite, called Linus or (22) Kalliope I Linus. It is quite large – about 28 km in diameter – and would be a sizeable asteroid by itself. It orbits about 1100 km from the center of Kalliope, equivalent to about 13.2 Kalliope radii.^[3]Linus was discovered on 29 August 2001 byJean-Luc MargotandMichael E. Brown,while another team led by William Merline also independently detected the moon 3 days later.^[6]^[7]

First stellar occultation

On 7 November 2006, the first stellar occultation by the satellite of an asteroid (Linus) was successfully observed by a group of Japanese observers^[4]according to a prediction that was made just one day before by Berthier et al.^[12]based on more than 5 years of regular observations of Kalliope binary system usingadaptive opticssystems on ground-based telescopes. The observedchordsof Linus give a unique opportunity to estimate the size of the moonlet which was estimated to 20–28 km.

Notes

^Flattening derived from the maximum aspect ratio (c/a): $f=1-{\frac {c}{a}}$ ,where (c/a) =0.59±0.02.^[5]

References

^"calliope".Oxford English Dictionary(Online ed.).Oxford University Press.(Subscription orparticipating institution membershiprequired.)
^^a ^b ^c ^d ^e ^f ^g"JPL Small-Body Database Browser: 22 Kalliope"(2010-06-02 last obs).Retrieved22 July2010.
^^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^jDescamps, P.; Marchis, F.; et al. (2008). "New determination of the size and bulk density of the binary asteroid 22 Kalliope from observations of mutual eclipses".Icarus.196(2): 578–600.arXiv:0710.1471.Bibcode:2008Icar..196..578D.doi:10.1016/j.icarus.2008.03.014.S2CID 118437111.
^^a ^bM. Sôma, et al. (2006). "'Occultation by Kalliope (22) and its satellite Linus ".Central Bureau Electronic Telegrams.732:1.Bibcode:2006CBET..732....1S.
^^a ^b ^c ^d ^eVernazza, P.; et al. (October 2021)."VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis".Astronomy & Astrophysics.654:A56.Bibcode:2021A&A...654A..56V.doi:10.1051/0004-6361/202141781.hdl:10261/263281.S2CID 239104699.
^^a ^b ^c ^d ^eJ.L. Margot & M.E. Brown (2003). "A Low-Density M-type Asteroid in the Main Belt".Science.300(5627): 1939–1942.Bibcode:2003Sci...300.1939M.doi:10.1126/science.1085844.PMID 12817147.S2CID 5479442.
^^a ^b ^c ^d ^eF. Marchis (2003). "A three-dimensional solution for the orbit of the asteroidal satellite of 22 Kalliope".Icarus.165(1): 112–120.Bibcode:2003Icar..165..112M.doi:10.1016/S0019-1035(03)00195-7.
^"EAR-A-5-DDR-TAXONOMY-V6.0".Planetary Data System.Archived fromthe originalon 17 December 2015.Retrieved16 April2018.
^A.S. Rivkin (2000). "The nature of M-class asteroids from 3-micron observations".Icarus.145(2): 351–368.Bibcode:2000Icar..145..351R.doi:10.1006/icar.2000.6354.
^D.F. Lupishko (1982). "UBV photometry of the M-type asteroids 16 Psyche and 22 Kalliope".Solar System Research.16:75.Bibcode:1982AVest..16..101L.
^M. Kaasalainen (2002)."Models of Twenty Asteroids from Photometric Data"(PDF).Icarus.159(2): 369–395.Bibcode:2002Icar..159..369K.doi:10.1006/icar.2002.6907.
^J. Berthier, et al. (2004). "'Prediction of stellar occultations by satellite of asteroids ".AAS/Division for Planetary Sciences Meeting Abstracts #36.32(23): 1142.Bibcode:2004DPS....36.3223B.

External links

Lightcurve plot of 22 Kalliope,Palmer Divide Observatory,B. D. Warner(2007)
orbit diagram for Linus
A different VLT image of Kalliope and Linus
(22) Kalliope,datasheet, johnstonsarchive.net
Asteroids with Satellites,Robert Johnston, johnstonsarchive.net
[1],Prediction and Reduction of Stellar Occultations of Binary Asteroids
22 KalliopeatAstDyS-2, Asteroids—Dynamic Site
- Ephemeris·Observation prediction·Orbital info·Proper elements·Observational info
22 Kalliopeat theJPL Small-Body Database
- Close approach·Discovery·Ephemeris·Orbit viewer·Orbit parameters·Physical parameters

[8] Flattening derived from the maximum aspect ratio (c/a): $f=1-{\frac {c}{a}}$ ,where (c/a) =0.59±0.02.^[5]

[1] "calliope".Oxford English Dictionary(Online ed.).Oxford University Press.(Subscription orparticipating institution membershiprequired.)

[jpl-2] ^^a ^b ^c ^d ^e ^f ^g"JPL Small-Body Database Browser: 22 Kalliope"(2010-06-02 last obs).Retrieved22 July2010.

[Descamps2008-3] ^^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^jDescamps, P.; Marchis, F.; et al. (2008). "New determination of the size and bulk density of the binary asteroid 22 Kalliope from observations of mutual eclipses".Icarus.196(2): 578–600.arXiv:0710.1471.Bibcode:2008Icar..196..578D.doi:10.1016/j.icarus.2008.03.014.S2CID 118437111.

[Soma06-4] M. Sôma, et al. (2006). "'Occultation by Kalliope (22) and its satellite Linus ".Central Bureau Electronic Telegrams.732:1.Bibcode:2006CBET..732....1S.

[VLT-5] Vernazza, P.; et al. (October 2021)."VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis".Astronomy & Astrophysics.654:A56.Bibcode:2021A&A...654A..56V.doi:10.1051/0004-6361/202141781.hdl:10261/263281.S2CID 239104699.

[Margot03-6] J.L. Margot & M.E. Brown (2003). "A Low-Density M-type Asteroid in the Main Belt".Science.300(5627): 1939–1942.Bibcode:2003Sci...300.1939M.doi:10.1126/science.1085844.PMID 12817147.S2CID 5479442.

[Marchis03-7] F. Marchis (2003). "A three-dimensional solution for the orbit of the asteroidal satellite of 22 Kalliope".Icarus.165(1): 112–120.Bibcode:2003Icar..165..112M.doi:10.1016/S0019-1035(03)00195-7.

[9] "EAR-A-5-DDR-TAXONOMY-V6.0".Planetary Data System.Archived fromthe originalon 17 December 2015.Retrieved16 April2018.

[Rivkin00-10] A.S. Rivkin (2000). "The nature of M-class asteroids from 3-micron observations".Icarus.145(2): 351–368.Bibcode:2000Icar..145..351R.doi:10.1006/icar.2000.6354.

[Lupishko82-11] D.F. Lupishko (1982). "UBV photometry of the M-type asteroids 16 Psyche and 22 Kalliope".Solar System Research.16:75.Bibcode:1982AVest..16..101L.

[Kaasalainen02-12] M. Kaasalainen (2002)."Models of Twenty Asteroids from Photometric Data"(PDF).Icarus.159(2): 369–395.Bibcode:2002Icar..159..369K.doi:10.1006/icar.2002.6907.

[Berthier04-13] J. Berthier, et al. (2004). "'Prediction of stellar occultations by satellite of asteroids ".AAS/Division for Planetary Sciences Meeting Abstracts #36.32(23): 1142.Bibcode:2004DPS....36.3223B.

[1]

[2]

[3]

[4]

[5]

[6]

[7]

[a]

[8]

[9]

[10]

[11]

[12]