24827 Maryphil

Last updated

24827 Maryphil
Discovery  [1]
Discovered by T. B. Spahr
Discovery site Catalina Stn.
Discovery date2 September 1995
Designations
(24827) Maryphil
Named after
Mary & Phil Spahr  [2]
(discoverer's parents)
1995 RA
main-belt  ·(inner)
Phocaea   [3] [4] [5]
Orbital characteristics   [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 22.09 yr (8,067 days)
Aphelion 2.8925 AU
Perihelion 1.7982 AU
2.3453 AU
Eccentricity 0.2333
3.59 yr (1,312 days)
31.688°
0° 16m 27.84s / day
Inclination 22.946°
303.03°
58.680°
Physical characteristics
Mean diameter
5.948±0.403 km [6]
6.72±0.19 km [7]
6.96 km (calculated) [3]
11.653±0.005 h [8] [lower-alpha 1]
0.23 (assumed) [3]
0.236±0.014 [7]
0.315±0.028 [6]
S Q   [9]  · S (assumed) [3]
13.00 [3] [6]  ·13.10 [1] [7]
13.37±0.32 [9]

    24827 Maryphil, provisional designation 1995 RA, is a stony Phocaea asteroid from the inner regions of the asteroid belt, approximately 6 kilometers in diameter. It was discovered on 2 September 1995, by American astronomer Timothy Spahr at the Catalina Station near Tucson, Arizona, who named it for his parents, Mary & Phil Spahr. [2]

    Contents

    Orbit and classification

    Maryphil is a core member of the Phocaea family ( 701 ), [3] [4] [5] a prominent family of stony asteroids with their largest members being 25 Phocaea and 587 Hypsipyle. [10] : 23  Unlike this asteroid, many members of the relatively eccentric Phocaea family are Mars-crossing asteroids.

    This asteroid orbits the Sun in the inner asteroid belt at a distance of 1.8–2.9  AU once every 3 years and 7 months (1,312 days; semi-major axis of 2.35 AU). Its orbit has an eccentricity of 0.23 and an inclination of 23° with respect to the ecliptic. [1]

    The body's observation arc begins at the discovering Catalina Station on 30 August 1992, just three nights prior to its official discovery observation. [2]

    Physical characteristics

    Pan-STARRS ' photometric survey characterized Maryphil as an S-type and Q-type asteroid, [9] while the Collaborative Asteroid Lightcurve Link (CALL) assumes it to be a common S-type, [3] which is also the overall spectral type form members of the Phocaea family. [10] : 23 

    Rotation period

    In November 2006, a rotational lightcurve of Maryphil was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of 11.653 hours with a brightness amplitude of 0.44 magnitude ( U=3- ). [8] [lower-alpha 1]

    Diameter and albedo

    According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Maryphil measures 5.948 and 6.72 kilometers in diameter and its surface has an albedo of 0.236 and 0.315, respectively. [6] [7] CALL assumes a standard albedo for Phocaea asteroids of 0.23, and calculates a diameter of 6.96 kilometers based on an absolute magnitude of 13.0. [3]

    Naming

    This minor planet was named by the discoverer Timothy Spahr in honor of his supportive parents, Mary Clark (born 1938) and Phil Spahr (born 1938). The official naming citation was published by the Minor Planet Center on 3 July 2012 ( M.P.C. 79910). [11]

    Notes

    1. 1 2 Lightcurve plot of (24827) Maryphil by Brian D. Warner at Palmer Divide Observatory (2006) rotation period 11.653±0.005 hours with a brightness amplitude of 0.44±0.02 mag. Summary figure at the LCDB.

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    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 24827 Maryphil (1995 RA)" (2017-09-30 last obs.). Jet Propulsion Laboratory . Retrieved 31 January 2018.
    2. 1 2 3 "24827 Maryphil (1995 RA)". Minor Planet Center. Retrieved 31 January 2018.
    3. 1 2 3 4 5 6 7 8 "LCDB Data for (24827) Maryphil". Asteroid Lightcurve Database (LCDB). Retrieved 31 January 2018.
    4. 1 2 "Asteroid 24827 Maryphil – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 29 October 2019.
    5. 1 2 "Asteroid 24827 Maryphil – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 29 October 2019.
    6. 1 2 3 4 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. S2CID   46350317.
    7. 1 2 3 4 Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117.
    8. 1 2 Warner, Brian D. (June 2007). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory - September-December 2006". The Minor Planet Bulletin. 34 (2): 32–37. Bibcode:2007MPBu...34...32W. ISSN   1052-8091.
    9. 1 2 3 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. S2CID   53493339.
    10. 1 2 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. S2CID   119280014.
    11. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 31 January 2018.
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