951 Gaspra

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951 Gaspra
951 Gaspra.jpg
NASA image of Gaspra; the colors are exaggerated
Discovery
Discovered by G. N. Neujmin
Discovery date July 30, 1916
Designations
Named after Gaspra
Alternative names SIGMA 45; A913 YA;
1955 MG1
Minor planet category Main belt (Flora family)
Orbital characteristics
Epoch 6 March 2006 (JD 2453800.5)
Aphelion 2.594 AU (388.102 Gm)
Perihelion 1.825 AU (272.985 Gm)
Semi-major axis 2.210 AU (330.544 Gm)
Eccentricity 0.174
Orbital period 3.28 a (1199.647 d)
Average orbital speed 19.88 km/s
Mean anomaly 53.057°
Inclination 4.102°
Longitude of ascending node 253.218°
Argument of perihelion 129.532°
Physical characteristics
Dimensions 18.2×10.5×8.9 km [1]
Mean radius 6.1 km[2]
Mass 2–3×1016 kg (estimate)
Mean density ~2.7 g/cm³ (estimate) [3]
Equatorial surface gravity ~0.002 m/s² (estimate)
Escape velocity ~0.006 km/s (estimate)
Rotation period 0.293 d (7.042 h) [4]
Albedo 0.22 [5]
Temperature ~181 K
max: 281 K (+8°C)
Spectral type S
Absolute magnitude (H) 11.46

951 Gaspra /ˈɡæsprə/ is an S-type asteroid that orbits very close to the inner edge of the asteroid belt. Gaspra was the first asteroid ever to be closely approached when it was visited by the Galileo spacecraft, which flew by on its way to Jupiter on 29 October 1991.

Characteristics[edit]

Successive images of a rotating Gaspra

Apart from a multitude of small craters, Gaspra has half a dozen large flat areas and concavities. One of these flat areas, (Dunne Regio), is a 5×7 km area which is flat to within 200 m. It is uncertain whether these are the result of impacts or whether they are instead facets formed when Gaspra broke off its parent asteroid. In the weak, lopsided gravity of Gaspra, impact craters would naturally take on such flat, lopsided shapes, making this determination difficult. The flat facets and concavities give Gaspra a very angular appearance.

Gaspra appears to be fairly olivine-rich among the S-type asteroids (the surface appears to contain olivine and pyroxene in the proportions 4:1 to 7:1[6]). There are no prominent albedo or color patterns, although a subtle color variation is seen across the surface (see image above).

Gaspra's surface lacks unambiguous craters of a size comparable to its radius, like those seen for example on 253 Mathilde. A probable reason is that the collision that produced the Flora family and Gaspra was relatively recent on an astronomical timescale, so that Gaspra has not yet had the opportunity to acquire many large craters since. Analysis of cratering rates suggests the age of the surface is between about 20 to 300 million years.[7]

Grooves about 100–300 m wide, up to 2.5 km long, and tens of meters deep are seen on Gaspra's surface, which may be related to Gaspra's formation along with the rest of the Flora family in an asteroid collision. Their presence also suggest that it is a single coherent body, rather than a rubble pile. The grooves were likely created by impacts that shattered the underlying rock. A system of much more prominent grooves is seen on the Martian moon Phobos. The pitted appearance of some grooves may suggest that the surface is covered by a regolith.[7]

The extensiveness of regolith on Gaspra and its presence overall is a matter of debate, and not fully understood. Visually, the somewhat subdued and mantled appearance suggests a substantial regolith. Also, correlations are seen between the subtle color variations and local topography, and it has been suggested that this is caused by the slow migration of regolith to lower areas. It is, however, difficult to explain the origin of a putative regolith. Firstly, Gaspra's escape velocity is very small, so small that it is difficult to understand how it could keep a significant portion of fragments ejected by impacts from escaping. This may be alleviated if Gaspra is a porous body or started with a large regolith, but one has to explain how the original regolith appeared. A possible resolution of the issue may be that Gaspra obtained a regolith during the Flora-family forming impact that also created Gaspra itself. Secondly, it has been estimated that the matter ejected by all the craters would be only enough to cover Gaspra with 10 m of regolith. However, some craters are much deeper than this without showing any structural difference on their walls.[8]

Gaspra's pole has been determined to point in the direction of RA 0h40m±10m, Declination 27±2°.[1] This is equivalent to ecliptic coordinates (β, λ) = (21°, 20°) and gives an axial tilt of 72°.

The Galileo flyby was too distant for a body of Gaspra's small size to noticeably affect Galileo's trajectory, so no information on Gaspra's mass was obtained. (Galileo also visited 243 Ida where it discovered a moon, allowing a mass estimate there.)

Gaspra's surface area has been calculated at about 525 km²,[1] which, for comparison, is about the size of Guam, or half the land area of Hong Kong.

Exploration[edit]

Gaspra and the Martian moons Phobos and Deimos, to scale

Gaspra was discovered by Russian astronomer G. N. Neujmin in 1916. Neujmin named it after Gaspra, a Black Sea retreat that was visited by his contemporaries, such as Gorky and Tolstoy.

Galileo flew by Gaspra on 29 October 1991, passing within 1,600 kilometers at a relative speed of about 8 kilometers per second (18,000 mph). 57 images were returned to Earth, the closest taken from a distance of 5300 km. The best images have a resolution of about 54 meters/pixel. The area around the southern pole was not seen during the flyby, but the remaining 80% of the asteroid was imaged.[7]

Because Gaspra's position was only known to within about 200 km before the encounter, and the camera's field of view was only about 5° across, Galileo would not know where to point to capture images of the asteroid once it was closer than 70,000 km. This would render the encounter not very interesting scientifically. To overcome this problem, a pioneering optical navigation campaign was implemented by the Galileo spacecraft team to reduce the uncertainty of Gaspra's position using images captured during the approach to Gaspra. This was spectacularly successful and allowed the spacecraft to obtain images from as close as 5300 km. At this closest range, the pointing was still not known quite accurately enough, but the camera actually took a 51 image mosaic so as to capture Gaspra on at least one image.[7] Similar optical navigation techniques have been used on all spacecraft flybys of asteroids since.

References[edit]

  1. ^ a b c P. C. Thomas, J. Veverka, D. Simonelli, P. Helfenstein, B. Carcich, M. J. S. Belton, M. E. Davies, C. Chapman (1994). "The Shape of Gaspra". Icarus 107 (1): 23–36. Bibcode:1994Icar..107...23T. doi:10.1006/icar.1994.1004. 
  2. ^ THOMAS P. C., VEVERKA J., SIMONELLI D., HELFENSTEIN P., BELTON M. J. S., DAVIES M. E., CHAPMAN C. – The Shape of Gaspra : Galileo's observations of 951 Gaspra (1994)
  3. ^ Krasinsky, G. A.; Pitjeva, E. V.; Vasilyev, M. V.; Yagudina, E. I. (July 2002). "Hidden Mass in the Asteroid Belt". Icarus 158 (1): 98–105. Bibcode:2002Icar..158...98K. doi:10.1006/icar.2002.6837. 
  4. ^ PDS lightcurve data
  5. ^ Supplemental IRAS Minor Planet Survey
  6. ^ J.C. Granahan F.P. Fanale, & M.S. Robinson (1994). "A Galileo Multi Spectral Instrument Analysis of 951 Gaspra". Abstracts of the 25th Lunar and Planetary Science Conference, held in Houston, TX, 14–18 March 1994: 453. 
  7. ^ a b c d Veverka, J.; Belton, M.; Klaasen, K.; Chapman, C. (1994). "Galileo's Encounter with 951 Gaspra: Overview". Icarus 107 (1): 2–17. Bibcode:1994Icar..107....2V. doi:10.1006/icar.1994.1002. 
  8. ^ M.J.S. Belton et al. (1992). "Galileo Encounter with 951 Gaspra: First Pictures of an Asteroid" (abstract). Science 257 (5077): 1647. Bibcode:1992Sci...257.1647B. doi:10.1126/science.257.5077.1647. PMID 17841160. 

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