706 Hirundo

Last updated

706 Hirundo
000706-asteroid shape model (706) Hirundo.png
Modelled shape of Hirundo from its lightcurve
Discovery  [1]
Discovered by J. Helffrich
Discovery site Heidelberg Obs.
Discovery date9 October 1910
Designations
(706) Hirundo
Pronunciation /hɪˈrʌndoʊ/ [2]
Named after
 Hirundo (swallows) [3]
(Genus of birds)
A910 TF ·1948 AE
1957 DA ·1977 QB
A924 WD ·1910 KX
Adjectives Hirundinian /hɪrənˈdɪniən/ [8]
Orbital characteristics   [4]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc 109.55 yr (40,014 d)
Aphelion 3.2601 AU
Perihelion 2.1987 AU
2.7294 AU
Eccentricity 0.1944
4.51 yr (1,647 d)
124.52°
0° 13m 6.96s / day
Inclination 14.431°
325.34°
31.090°
Physical characteristics
Mean diameter
22.027±0.005  h [12] [lower-alpha 1]
  • (92°, 66°) (λ1/β1) [6]
  • (244°, 54°) (λ2/β2) [6]
SMASS = Cgh   [4]

    706 Hirundo ( prov. designation:A910 TFor1910 KX) is an elongated background asteroid, located in the central region of the asteroid belt. It was discovered by German astronomer Joseph Helffrich at the Heidelberg Observatory on 9 October 1910. [1] The carbonaceous C-type asteroid (Cgh) has a rotation period of 22.0 hours and measures approximately 30 kilometers (19 miles) in diameter. It was named after the bird genus Hirundo , commonly known as swallows. [3]

    Contents

    Orbit and classification

    Orbit of .mw-parser-output .legend{page-break-inside:avoid;break-inside:avoid-column}.mw-parser-output .legend-color{display:inline-block;min-width:1.25em;height:1.25em;line-height:1.25;margin:1px 0;text-align:center;border:1px solid black;background-color:transparent;color:black}.mw-parser-output .legend-text{} 706 Hirundo (2000-2020) Earth * Mars * Jupiter Animation of 706 Hirundo orbit 2000-2020.gif
    Orbit of    706 Hirundo (2000-2020)
       Earth ·   Mars ·  Jupiter

    Hirundo is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. [5] [6] [7]

    It orbits the Sun in the central asteroid belt at a distance of 2.2–3.3  AU once every 4 years and 6 months (1,647 days; semi-major axis of 2.73 AU). Its orbit has an eccentricity of 0.19 and an inclination of 14° with respect to the ecliptic. [4] The body's observation arc begins at Vienna Observatory on 16 October 1910, or six nights after its official discovery observation by Joseph Helffrich at Heidelberg. [1]

    Naming

    This minor planet was named after bird genus Hirundo , a group of passerines in the family Hirundinidae (swallows and martins). [3] "Hirundo" is Latin word for swallow. They are found all over the world with the exception of New Zealand and the polar regions. Known for their graceful flight and regular migrations, swallows feature a short bill with a wide gape, small weak feet, and typically a deeply forked tail. They feed on insects caught on the wing. The naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 ( H 71 ). [3]

    Physical characteristics

    In both the Bus–Binzel (SMASS-II) and the Bus–DeMeo classification, Hirundo is a carbonaceous C-type asteroid (Cgh). [4] [6] [13]

    Rotation period and poles

    In September 2000, a rotational lightcurve of Hirundo was obtained from photometric observations by American Brian Warner at the Palmer Divide Observatory ( 716 ) in Colorado. Lightcurve analysis gave a rotation period of 22.027±0.005 hours with a high brightness variation of 0.9±0.03 magnitude, indicative of an elongated shape ( U=3 ). [12] [lower-alpha 1] During the same opposition, Bill Holliday measures a period of (22.00±0.025  h ) and an amplitude of (0.75±0.02) magnitude at his River Oaks Observatory ( 915 ) in New Braunfels, Texas ( U=3 ). [14] Further observations by René Roy (2011), Patrice Le Guen (2018), and Anaël Wünsche and Raoul Behrend (2020) determined a period of (22.002±0.003 h), (22.0±0.5 h) and (22.00248 h) with an amplitude of (0.39±0.01), (0.68±0.05) and (0.15±0.04) magnitude, respectively ( U=3/2/n.a. ). [15]

    Two lightcurves, published in 2016, using modeled photometric data from the Lowell Photometric Database (LPD) and other sources, gave a concurring period of (22.0160±0.0005) and (22.0161±0.0001) hours, respectively. Each modeled lightcurve also determined two spin axes of (92°, 66°) and (244°, 54°), as well as (91°, 70°) and (250°, 45°) in ecliptic coordinates (λ, β), respectively. [6] [16] [17] [18]

    Diameter and albedo

    According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Hirundo measures (29.22±1.5), (29.36±0.79) and (30.819±0.553) kilometers in diameter and its surface has an albedo of (0.1721±0.019), (0.172±0.011) and (0.081±0.011), respectively. [9] [10] [11]

    The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0853 and a diameter of 28.70 kilometers based on an absolute magnitude of 11. [16] The WISE-team also published two alternative mean-diameters of (24.44±8.42  km ) and (24.72±4.69 km) with a corresponding albedos of (0.09±0.07) and (0.09±0.03). [6] [16]

    Notes

    1. 1 2 Lightcurve plot of 706 Hirundo, Palmer Divide Observatory (PDO), B. Warner (2000). Rotation period 22.027±0.005 hours with a brightness amplitude of 0.9±0.03 mag. Quality code is 3. Summary figures at the LCDB and PDO websites.

    Related Research Articles

    <span class="mw-page-title-main">251 Sophia</span> Main-belt asteroid

    251 Sophia is a stony background asteroid from the outer regions of the asteroid belt. It was discovered on 4 October 1885, by astronomer Johann Palisa at the Vienna Observatory in Austria. The S-type asteroid (S/L) has a rotation period of 20.2 hours and measures approximately 28 kilometers in diameter. It was named after Sophia von Seeliger, wife of German astronomer Hugo von Seeliger (1849–1924).

    <span class="mw-page-title-main">698 Ernestina</span>

    698 Ernestina is a background asteroid, approximately 27 kilometers in diameter, located in the outer regions of the asteroid belt. It was discovered on 5 March 1910, by German astronomer Joseph Helffrich at the Heidelberg-Königstuhl State Observatory. The presumed carbonaceous C-type asteroid has a rotation period of 5.0 hours. It was named after Ernst Wolf, son of German astronomer and prolific discoverer of minor planets, Max Wolf.

    <span class="mw-page-title-main">749 Malzovia</span>

    749 Malzovia is a stony background asteroid from the inner regions of the asteroid belt, approximately 11 kilometers in diameter. It was discovered on 5 April 1913, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The elongated S-type asteroid has a rotation period of 5.9 hours. It was named after Russian amateur astronomer Nikolai Maltsov who founded the discovering Simeïs Observatory in 1900.

    <span class="mw-page-title-main">791 Ani</span>

    791 Ani is a very large asteroid of the Meliboea family, located in the outer regions of the asteroid belt. It was discovered on 29 June 1914, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The dark carbonaceous C-type asteroid has a rotation period of 11.2 hours and measures approximately 65.7 × 103.5 kilometers, with a mean-diameter of 100 km (62 mi). It was named after the historic Armenian city of Ani.

    <span class="mw-page-title-main">803 Picka</span>

    803 Picka is a large and dark background asteroid from the outer regions of the asteroid belt. It was discovered on 21 March 1915, by Austrian astronomer Johann Palisa at the Vienna Observatory. The carbonaceous D-type asteroid has a rotation period of 5.1 hours and measures approximately 57 kilometers in diameter. It was named after Czech physician Friedrich Pick (1867–1921).

    <span class="mw-page-title-main">881 Athene</span>

    881 Athene is a stony background asteroid from the central region of the asteroid belt. It was discovered on 22 July 1917, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The likely elongated S/L-type asteroid has a rotation period of 13.9 hours and measures approximately 12 kilometers in diameter. It was named after Athena, the goddess of wisdom in Greek mythology.

    <span class="mw-page-title-main">896 Sphinx</span>

    896 Sphinx is a background asteroid from the inner regions of the asteroid belt, that measures approximately 13 kilometers in diameter. It was discovered on 1 August 1918, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid has a rotation period of 21.0 hours and is one of few low-numbered objects for which no spectral type has been determined. It was named after the Sphinx, a creature from Greek and Egyptian mythology.

    <span class="mw-page-title-main">908 Buda</span>

    908 Buda is a background asteroid from the inner regions of the asteroid belt, approximately 30 kilometers in diameter. It was discovered by German astronomer Max Wolf at the Heidelberg Observatory on 30 November 1918. The uncommon L-type asteroid has a rotation period of 14.6 hours. It was named after Buda, the smaller part of the Hungarian city of Budapest.

    <span class="mw-page-title-main">1010 Marlene</span>

    1010 Marlene is a carbonaceous background asteroid from the outer regions of the asteroid belt, approximately 47 kilometers in diameter. It was discovered on 12 November 1923, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid was named after German actress and singer Marlene Dietrich.

    <span class="mw-page-title-main">1017 Jacqueline</span>

    1017 Jacqueline is a dark background asteroid from the central regions of the asteroid belt. It was discovered on 4 February 1924, by Russian-French astronomer Benjamin Jekhowsky at the Algiers Observatory, Algeria, in North Africa. The carbonaceous C-type asteroid has a rotation period of 7.87 hours with a high brightness amplitude of 0.6 magnitude and measures approximately 39 kilometers in diameter. It was named after the French physicist and long-time pupil of the discoverer, Jacqueline Zadoc-Kahn Eisenmann (1904–1998).

    <span class="mw-page-title-main">1088 Mitaka</span> Asteroid

    1088 Mitaka is a bright background asteroid from the inner regions of the asteroid belt. It was discovered on 17 November 1927, by Japanese astronomer Okuro Oikawa at the old Tokyo Astronomical Observatory in Japan. The stony S-type asteroid has a notably short rotation period of 3.0 hours and measures approximately 15 kilometers in diameter. It was named after the Japanese village of Mitaka.

    1213 Algeria, provisional designation 1931 XD, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 32 kilometers in diameter. Discovered by Guy Reiss at Algiers Observatory in 1931, it was named after the North African country of Algeria.

    <span class="mw-page-title-main">1672 Gezelle</span>

    1672 Gezelle, provisional designation 1935 BD, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 27 kilometers in diameter. It was discovered on 29 January 1935, by Belgian astronomer Eugène Delporte at Royal Observatory of Belgium in Uccle, Belgium. It was later named after Flemish poet and Roman Catholic priest Guido Gezelle.

    <span class="mw-page-title-main">1841 Masaryk</span>

    1841 Masaryk (prov. designation: 1971 UO1) is a carbonaceous background asteroid from the outer region of the asteroid belt, approximately 46 kilometers in diameter. It was discovered on 26 October 1971, by Czech astronomer Luboš Kohoutek at Bergedorf Observatory in Hamburg, Germany. The asteroid was named after the first President of Czechoslovakia, Tomáš Garrigue Masaryk.

    <span class="mw-page-title-main">1299 Mertona</span>

    1299 Mertona is a bright background asteroid from the central region of the asteroid belt. It was discovered on 18 January 1934, by French astronomer Guy Reiss at Algiers Observatory, Algeria, in northern Africa. The likely stony asteroid with an unknown spectral type has a rotation period of 5.0 hours and measures approximately 14 kilometers in diameter. It was named after English astronomer Gerald Merton.

    <span class="mw-page-title-main">1444 Pannonia</span>

    1444 Pannonia is a carbonaceous background asteroid from the outer region of the asteroid belt, approximately 29 kilometers in diameter. It was discovered on 6 January 1938, by Hungarian astronomer György Kulin at Konkoly Observatory in Budapest, Hungary. It was named after the ancient province of the Roman Empire, Pannonia.

    <span class="mw-page-title-main">1484 Postrema</span>

    1484 Postrema, provisional designation 1938 HC, is a carbonaceous Postremian asteroid and namesake of the Postrema family from the central regions of the asteroid belt, approximately 41 kilometers in diameter. It was discovered on 29 April 1938, by Soviet astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The name "Postrema" celebrates the astronomer's last minor planet discovery.

    <span class="mw-page-title-main">1312 Vassar</span> Carbonaceous Alauda asteroid

    1312 Vassar, provisional designation 1933 OT, is a carbonaceous Alauda asteroid from the outer region of the asteroid belt, approximately 30 kilometers in diameter. It was discovered on 27 July 1933, by Belgian–American astronomer George Van Biesbroeck at Yerkes Observatory in Wisconsin, United States. The asteroid was named for the American Vassar College.

    1803 Zwicky, prov. designation: 1967 CA, is a stony Phocaea asteroid and binary system from the inner regions of the asteroid belt, approximately 10 kilometers in diameter. It was discovered on 6 February 1967, by Swiss astronomer Paul Wild at Zimmerwald Observatory near Bern, Switzerland. It was later named after Swiss astronomer Fritz Zwicky. The discovery of a 2.5-kilometer sized companion was announced on 8 March 2021.

    <span class="mw-page-title-main">1719 Jens</span>

    1719 Jens is a background asteroid from the central region of the asteroid belt, approximately 19 kilometers in diameter. It was discovered on 17 February 1950, by German astronomer Karl Reinmuth at Heidelberg Observatory in southern Germany. It was named after a grandson of the discoverer.

    References

    1. 1 2 3 4 5 "706 Hirundo (A910 TF)". Minor Planet Center. Retrieved 16 June 2020.
    2. ↑ "hirundine" . Oxford English Dictionary (Online ed.). Oxford University Press.(Subscription or participating institution membership required.)
    3. 1 2 3 4 Schmadel, Lutz D. (2007). "(706) Hirundo". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 68. doi:10.1007/978-3-540-29925-7_707. ISBN   978-3-540-00238-3.
    4. 1 2 3 4 5 6 "JPL Small-Body Database Browser: 706 Hirundo (A910 TF)" (2020-04-28 last obs.). Jet Propulsion Laboratory . Retrieved 16 June 2020.
    5. 1 2 "Asteroid 706 Hirundo – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 16 June 2020.
    6. 1 2 3 4 5 6 7 "Asteroid 706 Hirundo". Small Bodies Data Ferret. Retrieved 16 June 2020.
    7. 1 2 Zappalà, V.; Bendjoya, Ph.; Cellino, A.; Farinella, P.; Froeschle, C. (1997). "Asteroid Dynamical Families". NASA Planetary Data System: EAR-A-5-DDR-FAMILY-V4.1. Retrieved 16 June 2020.} (PDS main page)
    8. ↑ 'Our Chronicle', The Eagle, vol. XXVIII, 1907, p. 355
    9. 1 2 3 4 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T . Retrieved 16 June 2020.
    10. 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. (online, AcuA catalog p. 153)
    11. 1 2 3 4 Mainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R.; et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System: EAR-A-COMPIL-5-NEOWISEDIAM-V1.0. Bibcode:2016PDSS..247.....M . Retrieved 16 June 2020.
    12. 1 2 Warner, B. (March 2001). "Asteroid Photometry at the Palmer Divide Observatory: Results for 706 Hirundo, 957 Camelia, and 1719 Jens" (PDF). Minor Planet Bulletin. 28 (1): 4–5. Bibcode:2001MPBu...28....4W. Archived from the original (PDF) on 13 February 2020. Retrieved 16 June 2020.
    13. ↑ DeMeo, Francesca E.; Binzel, Richard P.; Slivan, Stephen M.; Bus, Schelte J. (July 2009). "An extension of the Bus asteroid taxonomy into the near-infrared" (PDF). Icarus. 202 (1): 160–180. Bibcode:2009Icar..202..160D. doi:10.1016/j.icarus.2009.02.005. Archived from the original on 17 March 2014. Retrieved 28 September 2020. (Catalog at PDS)
    14. ↑ Holliday, B. (June 2001). "Photometry of Asteroid 706 Hirundo, August and September 2000" (PDF). Minor Planet Bulletin. 28 (1): 22. Bibcode:2001MPBu...28...22H. Archived from the original (PDF) on 17 June 2020. Retrieved 16 June 2020.
    15. ↑ Behrend, Raoul. "Asteroids and comets rotation curves – (706) Hirundo". Geneva Observatory. Retrieved 16 June 2020.
    16. 1 2 3 "LCDB Data for (706) Hirundo". Asteroid Lightcurve Database (LCDB). Retrieved 16 June 2020.
    17. ↑ Hanuš, J.; Ďurech, J.; Oszkiewicz, D. A.; Behrend, R.; Carry, B.; Delbo, M.; et al. (February 2016). "New and updated convex shape models of asteroids based on optical data from a large collaboration network". Astronomy and Astrophysics. 586: A108. arXiv: 1510.07422 . Bibcode:2016A&A...586A.108H. doi:10.1051/0004-6361/201527441. ISSN   0004-6361. S2CID   119112278.
    18. ↑ Ďurech, J.; Hanuš, J.; Oszkiewicz, D.; Vančo, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics. 587: A48. arXiv: 1601.02909 . Bibcode:2016A&A...587A..48D. doi:10.1051/0004-6361/201527573. ISSN   0004-6361. S2CID   118427201.
    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.