4022 Nonna

4022 Nonna, provisional designation 1981 TL4, is a Vestian asteroid from the inner regions of the asteroid belt, approximately 4 kilometers (2.5 miles) kilometers in diameter. It was discovered on 8 October 1981, by Soviet–Russian astronomer Lyudmila Chernykh at the Crimean Astrophysical Observatory.[1] The asteroid was named after Soviet actress Nonna Mordyukova. The nearly fast rotator has an exceptionally low lightcurve-amplitude indicating a nearly spherical shape.[3]

4022 Nonna
Discovery [1]
Discovered byL. Chernykh
Discovery siteCrimea–Nauchnij
Discovery date8 October 1981
Designations
(4022) Nonna
Named after
Nonna Mordyukova [1]
(Soviet actress)
1981 TL4 · 1966 PC
1984 OJ
main-belt [1][2] · (inner)
Vestian [3][4]
Orbital characteristics [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc65.34 yr (23,865 d)
Aphelion2.6585 AU
Perihelion2.0576 AU
2.3580 AU
Eccentricity0.1274
3.62 yr (1,323 d)
99.638°
0° 16m 19.92s / day
Inclination5.0911°
278.34°
34.066°
Physical characteristics
Mean diameter
3.67±7.00 km[5]
7.13 km (calculated)[3]
2.5868±0.0002 h[lower-alpha 1]
2.5873±0.0003 h[lower-alpha 2][lower-alpha 3]
2.5877±0.0005 h[6][lower-alpha 4]
2.62±0.02 h[7][lower-alpha 5]
0.20 (assumed)[3]
0.907±0.440[5]
QV [8] · S (assumed)[3]
12.90[5] · 13.1[2][3]
13.45±0.47[8]

    Orbit and classification

    Nonna is a member of the Vesta family (401).[3][4] Vestian asteroids have a composition akin to cumulate eucrites (HED meteorites) and are thought to have originated deep within 4 Vesta's crust, possibly from the Rheasilvia crater, a large impact crater on its southern hemisphere near the South pole, formed as a result of a subcatastrophic collision. Vesta is the main belt's second-largest and second-most-massive body after Ceres.[9][10]

    It orbits the Sun in the inner main-belt at a distance of 2.1–2.7 AU once every 3 years and 7 months (1,323 days; semi-major axis of 2.36 AU). Its orbit has an eccentricity of 0.13 and an inclination of 5° with respect to the ecliptic.[2] The asteroid was first observed at Goethe Link Observatory in October 1952. The body's observation arc begins with its observation as 1966 PC at Crimea-Nauchnij in August 1966, more than 15 years prior to its official discovery observation.[1]

    Physical characteristics

    Nonna has been characterized as a Q- and V-type asteroid by Pan-STARRS' photometric survey,[8] while the Collaborative Asteroid Lightcurve Link (CALL) assumes it to be a common S-type asteroid.[3] The overall spectral type of Vestian asteroids is typically that of a V-type.[9]:23

    Rotation period

    Since 2006, several rotational lightcurves of Nonna have been obtained from photometric observations at Modra Observatory by astronomers Adrián Galád and Petr Pravec.[lower-alpha 1][lower-alpha 2][lower-alpha 3] Analysis of the best-rated lightcurve from September 2006 gave a rotation period of 2.5877 hours with a brightness variation of 0.077 magnitude (U=3).[6][lower-alpha 4] A measurement by French amateur astronomer René Roy gave a similar result of 2.62 hours, after using an alternative period solution.[7][lower-alpha 5] All lightcurves showed an unusually low amplitude which is indicative for a spheroidal shape. The asteroid's short period is close to that of a fast rotator.

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Nonna measures 3.67 kilometers in diameter and its surface has an exceptionally high albedo of 0.907.[5] Conversely, CALL assumes a standard stony albedo of 0.20 and calculates a much larger diameter of 7.13 kilometers based on an absolute magnitude of 13.1.[3]

    Naming

    This minor planet was named after Soviet cinema actress Nonna Mordyukova (1925–2008), a celebrated People's Artist of the USSR. The official naming citation was published by the Minor Planet Center on 25 August 1991 (M.P.C. 18645).[11]

    Notes
    1. Pravec (2010) web: lightcurve plot of (4022) Nonna with a rotation period 2.5868±0.0002 hours and a brightness amplitude of 0.10±0.01 mag from March 2010. Quality Code is 3. Summary figures at the LCDB and Pravec, P.; Wolf, M.; Sarounova, L. (2010) with data sheet
    2. Pravec (2016) web: lightcurve plot of (4022) Nonna with a rotation period 2.5873±0.0003 hours and a brightness amplitude of 0.09±0.01 mag from April 2016. Quality Code is 3. Summary figures at the LCDB and Pravec, P.; Wolf, M.; Sarounova, L. (2016) with data sheet
    3. Pravec (2017) lightcurve plot of (4022) Nonna with a rotation period of 2.5873±0.0001 hours and an amplitude of 0.088 mag, from October 2017. Ondrejov data obtained by the NEO Photometric Program and collaborating projects with data sheet
    4. Galad/Pravec (2006) lightcurve plot of (4022) Nonna with a rotation period of 2.578 hours and an amplitude of 0.077 mag, from September 2006. Ondrejov data obtained by the NEO Photometric Program and collaborating projects with data sheet
    5. Period by René Roy from August 2003, corrected by the LCDB. Original period reported: 1.31 hours; amended to 2.62 hours. LCDB-comment: "this seems unlikely and so the double period was entered for the details record." Quality code of 2-.
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    References
    1. "4022 Nonna (1981 TL4)". Minor Planet Center. Retrieved 19 March 2018.
    2. "JPL Small-Body Database Browser: 4022 Nonna (1981 TL4)" (2018-02-25 last obs.). Jet Propulsion Laboratory. Retrieved 19 March 2018.
    3. "LCDB Data for (4022) Nonna". Asteroid Lightcurve Database (LCDB). Retrieved 19 March 2018.
    4. "Asteroid 4022 Nonna – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 27 October 2019.
    5. Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8.
    6. Galád, Adrián; Pravec, Petr; Gajdos, Stefan; Kornos, Leonard; Világi, Jozef (October 2007). "Seven Asteroids Studied from Modra Observatory in the Course of Binary Asteroid Photometric Campaign". Earth. 101 (1–2): 17–25. Bibcode:2007EM&P..101...17G. doi:10.1007/s11038-007-9146-6.
    7. Behrend, Raoul. "Asteroids and comets rotation curves – (4022) Nonna". Geneva Observatory. Retrieved 19 March 2018.
    8. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007.
    9. Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). Identification and Dynamical Properties of Asteroid Families. Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
    10. Kelley, Michael S.; Vilas, Faith; Gaffey, Michael J.; Abell, Paul A. (September 2003). "Quantified mineralogical evidence for a common origin of 1929 Kollaa with 4 Vesta and the HED meteorites". Icarus. 165 (1): 215–218. Bibcode:2003Icar..165..215K. doi:10.1016/S0019-1035(03)00149-0.
    11. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 19 March 2018.

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