Sinope (moon)

Sinope /sɪˈnoʊpiː/ is a retrograde irregular satellite of Jupiter discovered by Seth Barnes Nicholson at Lick Observatory in 1914,[1] and is named after Sinope of Greek mythology.

Sinope
Sinope photographed by the Haute-Provence Observatory on 14 August 1998
Discovery [1]
Discovered byS. B. Nicholson
Discovery date21 July 1914
Designations
Designation
Jupiter IX
Pronunciation/sɪˈnoʊpiː/[2][3]
Named after
Σινώπη Sinōpē
AdjectivesSinopean[4] /saɪnəˈpiːən/[5]
Orbital characteristics [6]
23939000 km
Eccentricity0.250
−724.5 day
168.4°
Inclination158.1°
303.1°
346.4°
Satellite ofJupiter
Physical characteristics
Mean diameter
~38 km[7][8]
Mass7.5×1016 kg
Mean density
2.6 g/cm3 (assumed)[7]
~ 0.014 m/s2 (0.001 g)
~ 0.023 km/s
Albedo0.04[7][8]
Temperature~ 124 K
18.2[7]
11.1[9]

    Sinope did not receive its present name until 1975;[10][11] before then, it was simply known as Jupiter IX. It was sometimes called "Hades"[12] between 1955 and 1975.

    Sinope was the outermost known moon of Jupiter until the discovery of Megaclite in 2000. The most distant moon of Jupiter now known is S/2003 J 2.

    Orbit
    Pasiphae group.

    Sinope orbits Jupiter on a high-eccentricity and high-inclination retrograde orbit. Its orbit is continuously changing due to solar and planetary perturbations.[13] Sinope is believed to belong to the Pasiphae group of retrograde irregular moons.[8] However, given its mean inclination and different colour, Sinope could be also an independent object, captured independently, unrelated to the collision and break-up at the origin of the group.[14] The diagram illustrates Sinope's orbital elements in relation to other satellites of the group.

    Sinope is also known to be in a secular resonance with Jupiter, similar to Pasiphae. However, Sinope can drop out of this resonance and has periods of both resonant and non-resonant behaviour in time scales of 107 years.[15]

    Physical characteristics

    Sinope has an estimated diameter of 38 km (assuming an albedo of 0.04)[8] Sinope is red (colour indices B−V=0.84, R−V=0.46),[14] unlike Pasiphae, which is grey.

    Sinope's infrared spectrum is similar to those of D-type asteroids but different from that of Pasiphae.[16] These dissimilarities of the physical parameters suggest a different origin from the core members of the group.

    See also
    • Sinope in fiction

    References
    1. Nicholson, S. B. (1914). "Discovery of the Ninth Satellite of Jupiter". Publications of the Astronomical Society of the Pacific. 26: 197–198. Bibcode:1914PASP...26..197N. doi:10.1086/122336. PMC 1090718.
    2. "Sinope". Dictionary.com Unabridged. Random House.
    3. Noah Webster (1884) A Practical Dictionary of the English Language
    4. Sergey Vnukov (2010) "Sinopean Amphorae of the Roman Period", Ancient Civilizations from Scythia to Siberia 16
    5. Hector Stuart (1876) Ben Nebo, and Other Poems, p. 22
    6. S.S. Sheppard (2019), Moons of Jupiter, Carnegie Science, on line
    7. "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). 19 February 2015. Retrieved 28 February 2020.
    8. Sheppard, S. S.; and Jewitt, D. C.; An Abundant Population of Small Irregular Satellites Around Jupiter, Nature, Vol. 423 (May 2003), pp. 261-263
    9. "M.P.C. 111777" (PDF). Minor Planet Circular. Minor Planet Center. 25 September 2018. Retrieved 28 February 2020.
    10. Nicholson, S. B. (April 1939). "The Satellites of Jupiter". Publications of the Astronomical Society of the Pacific. 51 (300): 85–94. Bibcode:1939PASP...51...85N. doi:10.1086/125010. (in which he declines to name the recently discovered satellites (pp. 93–94))
    11. IAUC 2846: Satellites of Jupiter 1974 October (naming the moon)
    12. Payne-Gaposchkin, Cecilia; Katherine Haramundanis (1970). Introduction to Astronomy. Englewood Cliffs, N.J.: Prentice-Hall. ISBN 0-13-478107-4.
    13. Jacobson, R. A. (2000). "The orbits of outer Jovian satellites" (PDF). Astronomical Journal. 120 (5): 2679–2686. Bibcode:2000AJ....120.2679J. doi:10.1086/316817.
    14. Grav, T.; Holman, M. J.; Gladman, B. J.; and Aksnes, K.; Photometric Survey of the Irregular Satellites, Icarus, Vol. 166 (2003), pp. 33-45
    15. Nesvorný, D.; Beaugé, C. & Dones, L. (2004). "Collisional Origin of Families of Irregular Satellites". The Astronomical Journal. 127 (3): 1768–1783. Bibcode:2004AJ....127.1768N. doi:10.1086/382099.
    16. Grav, T.; Holman, M. J. (2004). "Near-Infrared Photometry of the Irregular Satellites of Jupiter and Saturn". The Astrophysical Journal. 605 (2): L141–L144. arXiv:astro-ph/0312571. Bibcode:2004ApJ...605L.141G. doi:10.1086/420881.
    This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.