3548 Eurybates

3548 Eurybates

Eurybates and its satellite Queta (circled) imaged by the Hubble Space Telescope in 2019–2020
Discovery[1]
Discovered by	C. J. van Houten I. van Houten-G. Tom Gehrels
Discovery site	Palomar Obs.
Discovery date	19 September 1973
Designations
MPC designation	(3548) Eurybates
Pronunciation	/jʊˈrɪbətiːz/[2]
Named after	Eurybates [3] (Greek mythology)
Alternative designations	1973 SO · 1954 CB 1957 JX · 1978 EE5 1985 TZ
Minor planet category	Jupiter trojan [1][4][5] Greek [6][7] Eurybates [7][8] binary
Adjectives	Eurybatian
Orbital characteristics[4]
Epoch 25 February 2023 (JD 2460000.5)
Uncertainty parameter 0
Earliest precovery date	9 February 1954[1]
Aphelion	5.680 AU
Perihelion	4.733 AU
Semi-major axis	5.206 AU
Eccentricity	0.0909
Orbital period (sidereal)	11.88 yr (4,339 d)
Mean anomaly	27.507°
Mean motion	0° 4m 58.682s / day
Inclination	8.054°
Longitude of ascending node	43.542°
Argument of perihelion	27.481°
Jupiter MOID	0.1092 AU
TJupiter	2.972
Physical characteristics
Dimensions	77.5 × 71.3 × 61.8 km[9]
Mean diameter	69.3±1.4 km (area equivalent)[9]
Mass	(1.51±0.03)×1017 kg[10]
Mean density	1.1±0.3 g/cm3[10]
Synodic rotation period	8.7027283±0.0000029 h[9]
Axial tilt	150° (wrt ecliptic)[9] 158° (wrt orbit)[9]
Pole ecliptic latitude	−60°[9]
Pole ecliptic longitude	320°[9]
Geometric albedo	0.044±0.003[9]
Spectral type	C[11][9] B–V = 0.739±0.026[9] V–R = 0.384±0.021[9] V–I = 0.355±0.015[9]
Apparent magnitude	16.2 to 18.1
Absolute magnitude (H)	9.800±0.007[9]

3548 Eurybates (/jʊˈrɪbətiːz/ yə-RIB-ə-teez) is a carbonaceous Jupiter trojan from the Greek camp and the parent body of the Eurybates family, approximately 68 kilometers (42 miles) in diameter. It is a target to be visited by the Lucy mission in August 2027. Discovered during the second Palomar–Leiden Trojan survey in 1973, it was later named after Eurybates from Greek mythology. This C-type asteroid is among the 60 largest known Jupiter trojans and has a rotation period of 8.7 hours. Eurybates has one kilometer-sized satellite, named Queta, that was discovered in images taken by the Hubble Space Telescope in September 2018.

Discovery

Eurybates 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. In 1951, it was first observed as 1954 CB at the Goethe Link Observatory, extending the asteroid's observation arc by 22 years prior to its official discovery observation at Palomar.^[1] Since the discovery of 588 Achilles by Max Wolf in 1906, more than 7,000 Jupiter trojans, with nearly 4,600 bodies in the Greek camp, have already been discovered.^[6]

Palomar–Leiden Trojan survey

While the discovery date aligns with the second Palomar–Leiden Trojan survey, Eurybates has not received a "T-2" prefixed survey designation, which was assigned for the discoveries made by the fruitful collaboration between the Palomar and Leiden observatories 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 the discovery of several thousand asteroids.^[12]

Orbit and classification

Eurybates is a dark Jupiter trojan asteroid orbiting in the leading Greek camp at Jupiter's L₄ Lagrangian point, 60° ahead of Jupiter's orbit in a 1:1 resonance (see Trojans in astronomy).^[6][7] It orbits the Sun at a distance of 4.7–5.7 AU once every 11 years and 10 months (4,321 days; semi-major axis of 5.19 AU). Its orbit has an eccentricity of 0.09 and an inclination of 8° with respect to the ecliptic.^[4]

Eurybates family

Eurybates is the parent body of the small Eurybates family (005),^[7][8] with 218 known members of carbonaceous and/or primitive composition.^[13]: 23 Only a few families have been identified among the Jovian asteroids; four of them in the Greek camp. This potentially collisional family was first characterized by Jakub Rozehnal and Miroslav Brož in 2011, and further described in 2014.^[14][15] Members of this family include the Jupiter trojans 5258 Rhoeo, 8060 Anius, 9818 Eurymachos, (163189) 2002 EU6, (287577) 2003 FE42 and 360072 Alcimedon.^[13]

Physical characteristics

Eurybates has been characterized as a carbonaceous C-type asteroid by both the Lucy mission team and Brian Warner's Lightcurve Data Base.^[5][11] The overall spectral type for members of the Eurybates family is that of a C- and P-type.^[13]: 23

Rotational lightcurves

In May 1992, a rotational lightcurve of Eurybates was obtained from photometric observations by Stefano Mottola and Maria Gonano–Beurer using the now decommissioned ESO 1-metre telescope at La Silla Observatory in northern Chile. Lightcurve analysis gave a rotation period of 8.711 hours with a brightness variation of 0.20 magnitude (U=3-).^[5][16] In October 2010, photometric observations by American astronomer Robert Stephens at the Goat Mountain Astronomical Research Station (G79) in California gave a concurring period of 8.73 hours and an amplitude of 0.19 magnitude (U=2+).^[5][17]

Eurybates has an axial tilt of 150° with respect to the ecliptic, making it a retrograde rotator.^[9]

Diameter and albedo

According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Eurybates measures between 63.89 and 72.14 kilometers in diameter and its surface has an albedo between 0.052 and 0.060.^[18][19][20] The Collaborative Asteroid Lightcurve Link agrees with IRAS, and derives an albedo of 0.0491 and a diameter of 72.08 kilometers with an absolute magnitude of 9.6.^[5]

Naming

This minor planet was named after Eurybates, the Ancient hero from Greek mythology, who was a herald for the Greek armies during the Trojan War.^[3] The official naming citation was published by the Minor Planet Center on 28 April 1991 (M.P.C. 18138).^[21]

Exploration

Lucy mission target

Eurybates is planned to be visited by the Lucy spacecraft which launched in 2021.^[22] The flyby is scheduled for 12 August 2027, and will approach the asteroid to a distance of 1,000 km (620 mi) at a relative velocity of 5.8 km/s (13,000 mph) and a solar phase angle of 81°.^[11]

Satellite

Queta

Discovery images of Queta taken by Hubble on 12–14 September 2018
Discovery[23]
Discovered by	Keith S. Noll et al.
Discovery date	12 September 2018
Designations
Designation	Eurybates I
Named after	Enriqueta Basilio, first woman torchbearer at the 1968 Summer Olympics
Alternative names	S/2018 (3548) 1
Orbital characteristics[10]
Epoch 12 September 2018 09:45:13 UT (JD 2458373.9064)
Semi-major axis	2350±11 km
Eccentricity	0.125±0.009
Orbital period (sidereal)	82.46±0.06 d
Inclination	155.0°±0.2° (wrt ecliptic)
Argument of perihelion	53°±3°
Satellite of	3548 Eurybates
Physical characteristics[24]
Mean diameter	1.2±0.4 km
Apparent magnitude	26.8[25]
Absolute magnitude (H)	18.25+0.8 −0.6[24]

Eurybates has one known satellite, named Queta after Mexican Olympic athlete Enriqueta Basilio.^[26] Provisionally designated S/2018 (3548) 1, the satellite was discovered by Keith S. Noll and colleagues in images taken with the Hubble Space Telescope in September 2018.^[25][27] Subsequent follow-up observations later confirmed the satellite's existence, and the discovery was announced on 9 January 2020. The satellite was given the name Queta on 15 October 2020, in accordance with the International Astronomical Union's Olympic athlete naming convention for small Jupiter trojans (H > 12). In the naming citation, Enriqueta Basilio was recognized as the first woman torchbearer at the 1968 Summer Olympics, analogous to the role of heralds like Eurybates.^[26]

Queta is extremely faint, with an apparent magnitude of ~26.77.^[25] It is at least 6,000 times fainter than Eurybates, suggesting that Queta is likely very small, about 1.2 ± 0.4 km (0.75 ± 0.25 mi) in diameter if it has the same albedo as Eurybates.^[24] The satellite has an orbital period of 82.46±0.06 days, with a semi-major axis of 2,350 ± 11 km (1,460.2 ± 6.8 mi) and low eccentricity of 0.125±009.^[10] It is probably a fragment of Eurybates since it is part of a known collisional family.^[28][10] The presence of the satellite does not pose any adverse effects on the Lucy mission, though it provides an additional object for the spacecraft to study during its flyby in 2027.^[29][28]

References

External links

• Long-term evolution of asteroid families among Jovian Trojans, Jakub Rozehnal and Miroslav Brož (2014)
• 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
• 3548 Eurybates at AstDyS-2, Asteroids—Dynamic Site
  • Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• 3548 Eurybates at the JPL Small-Body Database
  • Close approach · Discovery · Ephemeris · Orbit diagram · Orbital elements · Physical parameters