1647 Menelaus

1647 Menelaus /mɛnəˈleɪəs/ is a mid-sized Jupiter trojan from the Greek camp, approximately 42 kilometers (26 miles) in diameter. It was discovered on 23 June 1957 by American astronomer Seth Nicholson at the Palomar Observatory in California, and later named after the Spartan King Menelaus from Greek mythology.^[1][3] The dark asteroid has a rotation period of 17.7 hours.^[9] It is the principal body of the proposed Menelaus cluster, which encompasses several, mostly tentative Jovian asteroid families.

Menelaus is a dark Jovian asteroid in a 1:1 orbital resonance with Jupiter. It is located in the leading Greek camp at the Gas Giant's L₄ Lagrangian point, 60° ahead on its orbit (see Trojans in astronomy). Since the discovery of the first Jupiter trojan, 588 Achilles, by astronomer Max Wolf in 1906, more than 7000 Jovian asteroids have already been discovered.^[5]

It orbits the Sun at a distance of 5.1–5.3 AU once every 11 years and 11 months (4,347 days; semi-major axis of 5.21 AU). Its orbit has an eccentricity of 0.02 and an inclination of 6° with respect to the ecliptic.^[4] Menelaus was first imaged at Palomar in November 1951. This precovery extends the body's observation arc by more than 5 years prior to its official discovery observation.^[1]

In 1993, Andrea Milani suggested that Menelaus might be the parent body of an asteroid family based on a modified HCM-analysis.^[11]: 78 The finding was also mentioned by David Jewitt in 2004,^[12]: 12 who noted that the Menelaus family is the largest proposed dynamical family to exist among the Jupiter trojans, despite having only 8 members.^[a]

In 2008, Fernando Roig and Ricardo Gil-Hutton described this particular aggregation of Jupiter trojans as the "Menelaus clan", which, similar to the Flora family in the inner asteroid belt, is composed of several families (or subfamilies).^[13]: 9 In this publication, the Menelaus clan encompasses a dozen clusters, if the separation criteria used in the HCM analysis are sufficiently relaxed. The principal bodies of these proposed family-like clusters include: 1647 Menelaus, 3548 Eurybates, 1749 Telamon, 12973 Melanthios, 13062 Podarkes, 5436 Eumelos, 2148 Epeios, 4007 Euryalos, 4138 Kalchas, 3063 Makhaon and others.^[13]: 10

With the exception of the Eurybates family, which was studied in more detail by Jakub Rozehnal and Miroslav Brož in 2011 (also see 3548 Eurybates § Eurybates family), all other proposed families with their principal bodies in the Menelaus clan, including Menelaus itself,^[6] are tentative and not listed neither on the Asteroids—Dynamic Site (Milani and Knežević), nor included in the robust HCM-analysis by Nesvorný (also see Asteroid family § All families).^[14]: 23 Instead, these bodies are considered non-family asteroids of the Jovian background population.

This minor planet was named after the Greek mythological figure, Menelaus, husband of Helen of Troy, brother of Agamemnon, and king and leader of the Spartan contingent of the Greek army during the Trojan War. The discoverer followed the convention to name bodies located in the camp to the east of Jupiter after famous Greek heroes.

The Dictionary of Minor Planet Names also mentions that the lunar crater Menelaus was named after the Greek hero.^[3] However, based on the official International Astronomical Union–WGPSN nomenclature, it is named after Greek geometer and astronomer Menelaus of Alexandria (70–140).^[15] The official naming citation was published by the Minor Planet Center in June 1960 (M.P.C. 2019).^[16]

Menelaus is an assumed C-type, while most larger Jupiter trojans are D-type asteroids. It has a V–I color index of 0.866.^[9][10]

The Palomar Transient Factory in California obtained a rotational lightcurve of Menelaus from photometric observation in the R-band in October 2010. It gave a rotation period of 17.7390 hours with a brightness variation of 0.32 magnitude in the R-band (U=2).^[9][17] In February 2014, a refined period of 17.74±0.01 hours with an amplitude of 0.15 magnitude was determined by American astronomer Robert D. Stephens at the Center for Solar System Studies (U=3-).^[8][b]

According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Menelaus measures 42.72 kilometers in diameter and its surface has an albedo of 0.056.^[7] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous asteroids of 0.057 and calculates a diameter of 44.22 kilometers using an absolute magnitude of 10.5.^[9]

• Center for Solar System Studies, homepage
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Dictionary of Minor Planet Names, Google books
• Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center
• Asteroid 1647 Menelaus Archived 22 June 2018 at the Wayback Machine at the Small Bodies Data Ferret
• 1647 Menelaus at AstDyS-2, Asteroids—Dynamic Site
  • Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• 1647 Menelaus at the JPL Small-Body Database
  • Close approach · Discovery · Ephemeris · Orbit viewer · Orbit parameters · Physical parameters