4022 Nonna

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4022 Nonna
Discovery [1]
Discovered byL. Chernykh
Discovery siteCrimea–Nauchnij
Discovery date8 October 1981
Designations
MPC designation
(4022) Nonna
Named after
Nonna Mordyukova [1]
(Soviet actress)
1981 TL4 · 1966 PC
1984 OJ
Minor planet category
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]
Synodic rotation period
2.5868±0.0002 h[a]
2.5873±0.0003 h[b][c]
2.5877±0.0005 h[6][d]
2.62±0.02 h[7][e]
0.20 (assumed)[3]
0.907±0.440[5]
QV [8] · S (assumed)[3]
Absolute magnitude (H)
12.90[5] · 13.1[2][3]
13.45±0.47[8]

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]

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.[a][b][c] 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][d] A measurement by French amateur astronomer René Roy gave a similar result of 2.62 hours, after using an alternative period solution.[7][e] 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. ^ a b 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. ^ a b 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. ^ a b 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. ^ a b 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. ^ a b 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-.

References[]

  1. ^ a b c d e "4022 Nonna (1981 TL4)". Minor Planet Center. Retrieved 19 March 2018.
  2. ^ a b c d "JPL Small-Body Database Browser: 4022 Nonna (1981 TL4)" (2018-02-25 last obs.). Jet Propulsion Laboratory. Retrieved 19 March 2018.
  3. ^ a b c d e f g h i "LCDB Data for (4022) Nonna". Asteroid Lightcurve Database (LCDB). Retrieved 19 March 2018.
  4. ^ a b "Asteroid 4022 Nonna – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 27 October 2019.
  5. ^ a b c d 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. ^ a b 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. ^ a b Behrend, Raoul. "Asteroids and comets rotation curves – (4022) Nonna". Geneva Observatory. Retrieved 19 March 2018.
  8. ^ a b c 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. ^ a b 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.

External links[]

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