44 Nysa
Lightcurve-based 3D-model of Nysa
Discovery
Discovered byH. Goldschmidt
Discovery date27 May 1857
Designations
(44) Nysa
Pronunciation/ˈnaɪsə/[1]
Named after
Nysa
1977 CE
Main belt (Nysa)
AdjectivesNysian /ˈnɪsiən/[2][3]
Orbital characteristics[4]
Epoch 2008-05-14 (JD 2454600.5)
Aphelion2.78291235 AU (416.3 Gm)
Perihelion2.06469721 AU (308.9 Gm)
2.42380478 AU (362.6 Gm)
Eccentricity0.148158617 ± 5.7499e-08
3.77 yr
118.743236 ± 2.4281e-05°
Inclination3.7028885 ± 6.2628e-06°
131.59519 ± 1.0657e-04°
342.52066 ± 1.0904e-04°
Physical characteristics
Dimensions113±10 × 67±10 × 65±12 km[5]
Mass3.7×1017 kg
Mean density
2.0 g/cm3
6.421417 ± 0.000001 h[6]
+58 ± 3° [6]
98 ± 2° [6]
0.44 ± 0.10 (vis.)[5]
0.19 ± 0.06 (rad.)[5]
E[6]
8.83 to 12.46
7.03 [4]
0.09" to 0.026"

    Nysa (minor planet designation: 44 Nysa) is a large and very bright main-belt asteroid, and the brightest member of the Nysian asteroid family. It is classified as a rare class E asteroid and is probably the largest of this type (though 55 Pandora is only slightly smaller).

    Discovery

    It was discovered by Hermann Goldschmidt on May 27, 1857, and named after the mythical land of Nysa in Greek mythology.

    Physical properties

    In 2002 Kaasalainen et al. used 63 lightcurves from the Uppsala Asteroid Photometric Catalog (UAPC) to construct a shape model of 44 Nysa. The shape model is conical, which they interpreted as indicating the asteroid may actually be a contact binary.[6]

    In 2003, Tanga et al. published results obtained from the Fine Guidance Sensor on the Hubble Space Telescope in which high-precision interferometry was performed on Nysa with the goal of a more accurate shape determination. Due to Hubble's orbit around the Earth, hours-long photometry sessions, as are normally used to resolve the asteroid's shape, were not possible. Instead, the team used interferometry on the asteroid at the time in its rotation when it would have its longest axis perpendicular to the Earth. Ellipsoidal shape models were then fit to the resulting data to determine an estimate of the asteroid's shape. Both single and double ellipsoid models were fit to the data with both providing approximately the same goodness of fit; leaving the team unable to differentiate between a single elongated object and the contact binary model put forth by Kaasalainen et al.[7] An observation of an occultation by 44 Nysa of TYC 6273-01033-1 from the Dutch amateur astronomer Harrie Rutten showed a two-phase reappearance on March 20, 2012. This confirms the conical shape or the binary nature of Nysa.

    In December 2006, Shepard et al. performed three days of radar observations on Nysa with the Arecibo radio telescope. The asteroid was found to have a high radar polarization value (μc) of 0.50 ± 0.2, a radar albedo () of 0.19 ± 0.06, and a visual albedo (pv) of 0.44 ± 0.10.[5] The albedo measurements were based on a shape model worked out at Arecibo. The best fit shape model as measured by the Arecibo team has parameters a/b = 1.7 ± 0.1, a/c = 1.6–1.9, with an a-axis of 113 ± 10 km; this gives an effective diameter of 79 ± 10 km, which is in agreement with the HST study by Tanga et al. in 2003.[5] The data gathered also showed signs of significant concavity in Nysa's structure, but the dip in the radar curves is not pronounced enough to indicate bifurcation, calling into question whether or not Nysa really is a contact binary.[5]

    Nysa has so far been reported occulting a star three times.

    Studies

    44 Nysa was in a study of asteroids using the Hubble FGS.[8] Asteroids studied include (63) Ausonia, (15) Eunomia, (43) Ariadne, (44) Nysa, and (624) Hektor.[8]

    See also

    References

    1. ↑ Noah Webster (1884) A Practical Dictionary of the English Language
    2. ↑ Katz (2004) The complete elegies of Sextus Propertius
    3. ↑ Stein (2004) Persephone Unveiled
    4. 1 2 "44 Nysa". JPL Small-Body Database. Jet Propulsion Laboratory. SPK-ID: 44.
    5. 1 2 3 4 5 6 Shepard, M.; et al. (May 2008). "Radar observations of E-class Asteroids 44 Nysa and 434 Hungaria". Icarus. 195 (1): 220–225. Bibcode:2008Icar..195..220S. doi:10.1016/j.icarus.2007.12.018.
    6. 1 2 3 4 5 Kaasalainen, M.; Torppa, J.; Piironen, J. (March 2002). "Binary structures among large asteroids". Astronomy and Astrophysics. 383 (3): L19–L22. Bibcode:2002A&A...383L..19K. doi:10.1051/0004-6361:20020015.
    7. ↑ Tanga, P.; et al. (April 2003). "Asteroid observations with the Hubble Space Telescope. II. Duplicity search and size measurements for 6 asteroids". Astronomy and Astrophysics. 401 (2): 733–741. Bibcode:2003A&A...401..733T. doi:10.1051/0004-6361:20030032.
    8. 1 2 Tanga, P.; Hestroffer, D.; Cellino, A.; Lattanzi, M.; Martino, M. Di; Zappalà, V. (1 April 2003). "Asteroid observations with the Hubble Space Telescope FGS". Astronomy & Astrophysics. 401 (2): 733–741. Bibcode:2003A&A...401..733T. doi:10.1051/0004-6361:20030032. ISSN 0004-6361.

    Further reading

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