20936 Nemrut Dagi

Last updated

20936 Nemrut Dagi
Discovery [1]
Discovered by C. J. van Houten
I. van Houten-G.
T. Gehrels
Discovery site Palomar Obs.
Discovery date13 May 1971
Designations
(20936) Nemrut Dagi
Named after
 Nemrut Dağı
(volcano in Turkey) [1]
4835 T-1 ·1953 CP
1992 SR
main-belt  ·(inner) [2]
Hungaria   [1]
Orbital characteristics [2]
Epoch 1 July 2021 (JD 2459396.5)
Uncertainty parameter 0
Observation arc 50.12 yr (18,308 d)
Aphelion 2.0419 AU
Perihelion 1.6671 AU
1.8545 AU
Eccentricity 0.1011
2.53 yr (922 d)
168.55°
0° 23m 25.08s / day
Inclination 18.599°
26.629°
324.45°
Physical characteristics
Mean diameter
  • 3.21±0.50  km [3]
  • 3.51±0.66 km [4]
  • 3.567±0.189 km [5]
3.2754±0.0005  h [6] [7]
  • 0.31±0.11 [3]
  • 0.43±0.14 [4]
  • 0.460±0.078 [5]
E/S   [7]
14.02 [1] [2]

    20936 Nemrut Dagi (provisional designation 4835 T-1) is a stony Hungaria asteroid and Mars-grazer from the innermost regions of the asteroid belt, approximately 3.5 kilometers (2.2 miles) in diameter. It was discovered on 13 May 1971, by Dutch astronomer couple Ingrid and Cornelis van Houten at Leiden, on photographic plates taken by Dutch–American astronomer Tom Gehrels at Palomar Observatory in California, United States. The asteroid has a rotation period of 3.28 hours, a likely spheroidal shape, and a high albedo typically seen among the enstatite-rich E-type asteroids. In 2012, it was named after the a dormant volcano Nemrut (Nemrut Dağı) in Turkey. [1]

    Contents

    Orbit and classification

    Nemrut Dagi belongs to the dynamical group of Hungaria asteroids, [1] which form the innermost dense concentration of asteroids in the Solar System. It orbits the Sun in the inner main-belt at a distance of 1.7–2.0  AU once every 2 years and 6 months (922 days; semi-major axis of 1.85 AU). Its orbit has an eccentricity of 0.10 and an inclination of 19° with respect to the ecliptic. [2] Nemrut Dagi is also an outer Mars-grazer, as its orbit has a perihelion (1.667 AU) slightly below the aphelion of Mars (1.67 AU), not crossing the Red Plant's osculating orbit. It is classified as an "inner main-belt asteroid" in the JPL's data base, where it would be labelled a Mars-crosser if it had a perihelion of 1.666 AU or less. [2] The asteroid's observation arc begins with its observation as 1953 CP at Palomar Observatory in February 1953, or 18 years prior to its official discovery in 1971. [1]

    Designation

    Survey designation

    Upon discovery, this minor planet was designated 4835 T-1. The survey designation means that it was the 4835th object discovered in the "T-1" series, which stands for the first Palomar–Leiden Trojan survey, named after the fruitful collaboration of the Palomar and Leiden Observatory in the 1960s and 1970s. Gehrels used Palomar's Samuel Oschin telescope (also known as the 48-inch Schmidt Telescope), and shipped the photographic plates to Ingrid and Cornelis van Houten at Leiden Observatory where astrometry was carried out. The trio are credited with several thousand asteroid discoveries. [8]

    Naming

    It was named after the dormant volcano Nemrut (Nemrut Dağı) in Turkey. It is the most western volcano of a group of volcanoes near Lake Van in Eastern Anatolia. The volcano is named after King Nimrod who is said to have ruled this area in about 2100 BC. The asteroid's name was proposed by German astronomer Joachim Schubart, [1] and its official naming citation was published by the Minor Planet Center on 6 April 2012 ( M.P.C. 79103). [9]

    Physical characteristics

    Lightcurves

    In December 2015, a rotational lightcurve of Nemrut Dagi was obtained by American astronomer Brian Warner at his CS3–Palmer Divide Station ( U82 ) in California. Lightcurve analysis gave a well-defined rotation period of 3.2754±0.0005 hours with a low brightness variation of 0.08±0.01 magnitude ( U=3 ), indicating that the body has a rather spheroidal shape. [6]

    This result supersedes previous observations. Warner obtained similar periods of 3.233±0.002 and an amplitude of 0.05±0.01 (November 2007, revised), [6] 3.321±0.002 hours and 0.15±0.02 (February 2011), [10] and 5.697±0.002 hours and 0.15±0.02 (November 2007), [11] with a quality code of U=2, 2 and 0, respectively. [7] The asteroid was also observed by American astronomer Brian A. Skiff during the Near-Earth Asteroid Photometric Survey (NEAPS) at Lowell Observatory, who obtained a period of 3.233±0.002 in February 2011, which he directly reported to the LCBD ( U=2 ). [lower-alpha 1] Additional observations by NEAPS were published in 2019, and gave a concurring period of 3.283±0.007, 3.285±0.004, and 3.274±0.003 ( U=2+,2+,2+ ). [12] In May 2019, observations by Robert Stephens at CS3 ( U81 ) determined a period of 3.328±0.002 ( U=2 ). [13] : 453 

    Diameter and albedo

    According to the surveys carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid has a mean-diameter of 3.21±0.50 km, 3.51±0.66 km, and 3.57±0.19 km with an exceptionally high albedo of 0.31±0.11, 0.43±0.14, and 0.460±0.078, respectively. [3] [4] [5] [14] A high albedo of 0.30 or more is typically seen among the bright E-type asteroids that are thought to be composed of enstatite, a mineral which is rich in Magnesium sulfite (MgS03). The Collaborative Asteroid Lightcurve Link assumed a standard albedo for a common S-type asteroid of 0.20, and calculates a larger diameter of 5.3 kilometers based on an absolute magnitude of 13.8. [7]

    Notes

    1. ↑ Skiff (2011) web: rotation period 3.293±0.001 hours with a brightness amplitude of 0.06 mag. Summary figures for (20936) Nemrut Dagi at Dagi Collaborative Asteroid Lightcurve Link (CALL)

    Related Research Articles

    850 Altona is a large background asteroid, approximately 77 kilometers in diameter, that is located in the outer region of the asteroid belt. It was discovered on 27 March 1916, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The X-type asteroid has a rotation period of 11.2 hours. It was named after the city of Altona near Hamburg, Germany.

    1025 Riema, provisional designation 1923 NX, is a bright Hungaria asteroid from the innermost regions of the asteroid belt, approximately 5 kilometers in diameter. It was discovered on 12 August 1923, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. The asteroid was named after ARI astronomer Johannes Riem.

    (12538) 1998 OH is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.8 kilometers in diameter. It was discovered on 19 July 1998, by astronomers of the Near-Earth Asteroid Tracking program at the Haleakala Observatory in Hawaii, United States. In 2019, the asteroid came within about 73 lunar distances of Earth.

    4031 Mueller, provisional designation 1985 CL, is a Hungaria asteroid from the inner regions of the asteroid belt, approximately 4 kilometers in diameter. It was discovered on 12 February 1985, by American astronomer Carolyn Shoemaker at Palomar Observatory, California, and named after astronomer Jean Mueller.

    3225 Hoag, provisional designation 1982 QQ, is a dynamical Hungaria asteroid from the innermost regions of the asteroid belt, approximately 5.5 kilometers in diameter. It was discovered on 20 August 1982, by American astronomer couple Carolyn and Eugene Shoemaker at the Palomar Observatory in California. The stony S/L-type asteroid has a short rotation period of 2.37 hours. It was named for American astronomer Arthur Hoag.

    5175 Ables, provisional designation 1988 VS4, is a bright Hungaria asteroid from the inner regions of the asteroid belt, approximately 5 kilometers in diameter. It was discovered by American astronomers Carolyn and Eugene Shoemaker at the U.S. Palomar Observatory, California, on 4 November 1988. It was named after American astronomer Harold Ables.

    4401 Aditi, provisional designation 1985 TB, is an eccentric, stony asteroid, classified as a near-Earth object and Amor asteroid, approximately 1.8 kilometers in diameter. It was discovered on 14 October 1985 by American astronomer Carolyn Shoemaker at Palomar Observatory in California, and later named after the Hindu goddess Aditi.

    5806 Archieroy, provisional designation 1986 AG1, is a stony Hungaria asteroid from the inner regions of the asteroid belt, approximately 6 kilometers in diameter. It was discovered on 11 January 1986, by American astronomer Edward Bowell at Lowell's Anderson Mesa Station near Flagstaff, Arizona. It is named after Scottish astrophysicist Archie Roy.

    3737 Beckman, provisional designation 1983 PA, is a stony asteroid and sizable Mars-crosser on an eccentric orbit from the inner regions of the asteroid belt, approximately 14 kilometers in diameter. It was discovered on 8 August 1983, by American astronomer Eleanor Helin at the Palomar Observatory in California. The S-type asteroid has a rotation period of 3.1 hours. It was named for American Chemist Arnold Beckman.

    7187 Isobe, provisional designation 1992 BW, is a likely binary Hungaria asteroid from the inner regions of the asteroid belt, approximately 5 kilometers in diameter. It was discovered on 30 January 1992, by American astronomer Eleanor Helin at Palomar Observatory in California, United States. It is named after Japanese astronomer Syuzo Isobe.

    1355 Magoeba, provisional designation 1935 HE, is a Hungaria asteroid and a suspected contact-binary from the innermost regions of the asteroid belt, approximately 5 kilometers in diameter. It was discovered on 30 April 1935, by English-born, South African astronomer Cyril Jackson at the Johannesburg Observatory in South Africa. The asteroid is named for Magoeba, a tribal chief in the South African Transvaal Province.

    4068 Menestheus is a dark Jupiter trojan from the Greek camp, approximately 67 kilometers in diameter. It was discovered on 19 September 1973, by Dutch astronomers Ingrid and Cornelis van Houten at Leiden, on photographic plates taken by Tom Gehrels at the Palomar Observatory in California, United States. The D-type asteroid belongs to the 60 largest Jupiter trojans and has a rotation period of 14.4 hours. It was named after the Athen leader Menestheus from Greek mythology.

    9165 Raup, provisional designation 1987 SJ3, is a stony Hungaria asteroid and exceptionally slow rotator from the inner regions of the asteroid belt, approximately 4.7 kilometers in diameter.

    3873 Roddy, provisional designation 1984 WB, is a stony Hungarian asteroid, Mars-crosser and suspected binary system, from the innermost regions of the asteroid belt, approximately 7 kilometers in diameter. It was discovered on 21 November 1984, by American astronomer Carolyn Shoemaker at the Palomar Observatory in California, United States. It was named after American astrogeologist David Roddy.

    2074 Shoemaker, provisional designation 1974 UA, is a stony Hungaria asteroid, Mars-crosser and suspected synchronous binary system from the innermost regions of the asteroid belt, approximately 4 kilometers in diameter. It was discovered on 17 October 1974, by astronomer Eleanor Helin at the Palomar Observatory. She named it after American astronomer Eugene Shoemaker.

    4440 Tchantchès, provisional designation 1984 YV, is a rather elongated Hungaria asteroid and a possible binary system from the inner regions of the asteroid belt, approximately 3 kilometers in diameter.

    <span class="mw-page-title-main">1600 Vyssotsky</span>

    1600 Vyssotsky, provisional designation 1947 UC, is a rare-type Hungaria asteroid and suspected interloper from the inner regions of the asteroid belt, approximately 7 kilometers in diameter. It was discovered on 22 October 1947, by American astronomer Carl Wirtanen at Lick Observatory in California, United States. It was named after astronomer Alexander Vyssotsky.

    (6382) 1988 EL is a stony Hungaria asteroid from the inner regions of the asteroid belt, approximately 5 kilometers in diameter. It was discovered on 14 March 1988, by American astronomer Jeffrey Alu at the U.S. Palomar Observatory, California.

    (90075) 2002 VU94 (provisional designation 2002 VU94) is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 2.5 kilometers in diameter. It was discovered on 13 November 2002, by astronomers of the Near-Earth Asteroid Tracking program at Palomar Observatory in California, United States. It is one of the largest potentially hazardous asteroids known.

    (15502) 1999 NV27 (provisional designation 1999 NV27) is a Jupiter trojan from the Trojan camp, approximately 53 kilometers (33 miles) in diameter. It was discovered on 14 July 1999, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. The dark Jovian asteroid has a rotation period of 15.1 hours and belongs to the 90 largest Jupiter trojans. It has not been named since its numbering in June 2000.

    References

    1. 1 2 3 4 5 6 7 8 "20936 Nemrut Dagi (4835 T-1)". Minor Planet Center. Retrieved 30 August 2021.
    2. 1 2 3 4 5 "JPL Small-Body Database Browser: 20936 Nemrut Dagi (4835 T-1)" (2021-06-27 last obs.). Jet Propulsion Laboratory . Retrieved 30 August 2021.
    3. 1 2 3 Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016). "NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos". The Astronomical Journal. 152 (3): 12. arXiv: 1606.08923 . Bibcode:2016AJ....152...63N. doi: 10.3847/0004-6256/152/3/63 .
    4. 1 2 3 Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv: 1509.02522 . Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. S2CID   9341381.
    5. 1 2 3 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.
    6. 1 2 3 Warner, Brian D. (April 2016). "Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2015 October-December" (PDF). The Minor Planet Bulletin. 43 (2): 137–140. Bibcode:2016MPBu...43..137W. ISSN   1052-8091. PMC   7243998 . PMID   32455371 . Retrieved 30 August 2021. Lightcurve plot
    7. 1 2 3 4 "LCDB Data for (20936) Nemrut Dagi". Asteroid Lightcurve Database (LCDB). Retrieved 26 January 2016.
    8. ↑ "Minor Planet Discoverers". Minor Planet Center. 23 March 2016. Retrieved 4 April 2016.
    9. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 4 July 2017.
    10. ↑ Warner, Brian D. (July 2011). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2010 December- 2011 March" (PDF). The Minor Planet Bulletin. 38 (3): 142–149. Bibcode:2011MPBu...38..142W. ISSN   1052-8091 . Retrieved 30 August 2021.
    11. ↑ Warner, Brian D. (June 2008). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory: September–December 2007" (PDF). The Minor Planet Bulletin. 35 (2): 67–71. Bibcode:2008MPBu...35...67W. ISSN   1052-8091 . Retrieved 30 August 2021.
    12. ↑ Skiff, Brian A.; McLelland, Kyle P.; Sanborn, Jason J.; Pravec, Petr; Koehn, Bruce W. (October 2019). "Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS): Paper 4". Minor Planet Bulletin. 46 (4): 458–503. Bibcode:2019MPBu...46..458S. ISSN   1052-8091.
    13. ↑ Stephens, Robert D.; Warner, Brian D. (October 2019). "Main-belt Asteroids Observed from CS3: 2019 April to June" (PDF). Minor Planet Bulletin. 46 (4): 449–456. Bibcode:2019MPBu...46..449S. ISSN   1052-8091. Archived from the original (PDF) on 8 June 2021. Retrieved 30 August 2021. Lightcurve plot
    14. ↑ "Asteroid 20936 Nemrut Dagi – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 30 August 2021.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.