Wikipedia

(307261) 2002 MS4

(307261) 2002 MS4 (provisional designation 2002 MS4) is a large trans-Neptunian object in the Kuiper belt, which is a region of icy planetesimals beyond Neptune. It was discovered on 18 June 2002 by Chad Trujillo and Michael Brown during their search for bright, Pluto-sized Kuiper belt objects at Palomar Observatory. To within measurement uncertainties, 2002 MS4, 2002 AW197, and 2013 FY27 have a diameter close to 800 km (500 mi), which makes them the largest unnamed objects in the Solar System. 2002 MS4 is large enough that astronomers consider it a possible dwarf planet.

(307261) 2002 MS4
2002 MS4 imaged by the Hubble Space Telescope on 9 April 2006
Discovery[1]
Discovered byChadwick A. Trujillo
Michael E. Brown
Discovery sitePalomar Obs.
Discovery date18 June 2002
Designations
2002 MS4
TNO[2] · cubewano (hot)[3]: 56 
distant[1] · Scat-Ext[4]
Orbital characteristics (barycentric)[5][2]
Epoch 25 February 2023 (JD 2460000.5)
Uncertainty parameter 2
Observation arc66.22 yr (24,188 d)
Earliest precovery date8 April 1954
Aphelion47.801 AU
Perihelion35.677 AU
41.739 AU
Eccentricity0.14524
269.48 yr (98,429 d)
226.844°
0° 0m 13.167s / day
Inclination17.693°
216.075°
≈ 10 June 2123[6]
±0.6 days[2]
214.575°
Physical characteristics
Dimensions(823±20) × (770±34) km (projected)[7]
796±24 km[7]
Flattening≥0.066±0.034[7]: 5 
14.251 h[8]: 5, 54 
7.33 h or 10.44 h (single-peaked)[9]: 158 [a]
0.100±0.025[7]: 8  or 0.098±0.004[10]: 2  (geometric)
0.039±0.005 (Bond)[10]: 23 
Temperature65 K[11]
B−V=0.69±0.02[12]: 6 
V−R=0.38±0.02
B−R=1.07±0.02
20.5[13]
3.56±0.03[8]: 62, 74 
3.63±0.05[7]: 8 
3.62[2][1]

The surface of 2002 MS4 is dark gray and is composed of water and carbon dioxide ices. 2002 MS4 has been observed through stellar occultations, which have revealed massive topographic features along the outline of its shape. These features include a mountain-like peak that is 25 km (16 mi) tall and a crater-like depression that is 320 km (200 mi) wide and 45 km (28 mi) deep. 2002 MS4's topographic features are among the tallest and deepest known for Solar System bodies.

History

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Discovery

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2002 MS4 was discovered on 18 June 2002 by astronomers Chad Trujillo and Michael Brown at Palomar Observatory in San Diego County, California, United States.[1] The discovery formed part their Caltech Wide Area Sky Survey for bright, Pluto-sized Kuiper belt objects using the observatory's 1.22-meter (48 in) Samuel Oschin telescope with its wide-field CCD camera, which was operated jointly with the nightly Near Earth Asteroid Tracking program at Palomar.[14]: 100  This survey was responsible for the discovery of several other large objects beyond Neptune, which includes the dwarf planets Eris, Sedna, and Quaoar.[15]: 214 

2002 MS4 was found through manual vetting of potential moving objects identified by the team's automatic image-searching software.[14]: 101  It was among the fainter objects detected, just below the survey's limiting magnitude with an observed brightness of magnitude 20.9.[14]: 99, 103  Follow-up observations were conducted two months later with Palomar Observatory's 1.52-meter (60 in) telescope on 8 August 2002.[16] The discovery was announced by the Minor Planet Center on 21 November 2002 and the object was given the minor planet provisional designation of 2002 MS4.[16]

 
The 1.2-meter Samuel Oschin telescope that was used to discover 2002 MS4 at Palomar Observatory
 
Discovery images of 2002 MS4 from 18 June 2002

Further observations

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Since receiving follow-up in August 2002, 2002 MS4 remained unobserved for more than nine months until it was recovered by Trujillo at Palomar Observatory on 29 May 2003, followed by observations by Wolf Bickel at Bergisch Gladbach Observatory in Germany in June 2003.[17] These recovery observations significantly reduced the uncertainty of 2002 MS4's orbit, allowing for further extrapolation of its position backwards in time for identification in precovery observations.[18] Seven precovery observations from Digitized Sky Survey plates were identified by astronomer Andrew Lowe in 2007; the earliest of these was taken on 8 April 1954 by Palomar Observatory.[18][19]: 42  As of 2023, 2002 MS4 has been observed for over 68 years, or about 25% of its orbital period.[2][1]

Numbering and naming

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2002 MS4 received its permanent minor planet catalog number of 307261 from the Minor Planet Center on 10 December 2011.[18][20]: 292  As of yet, it remains unnamed and the discoverers' privilege for naming this object expired ten years after its numbering.[1][21]: 6  Per naming guidelines by the International Astronomical Union's Working Group for Small Bodies Nomenclature, 2002 MS4 is open for name suggestions that pertain to creation myths, as required for Kuiper belt objects in general.[21]: 8 

Orbit and classification

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2002 MS4 is a trans-Neptunian object (TNO) orbiting the Sun beyond Neptune with an orbital period of 269 years.[5][b] Its semi-major axis or average orbital distance from the Sun is 41.7 astronomical units (AU), with a moderate[3]: 45  orbital eccentricity of 0.15.[5] In its eccentric orbit, 2002 MS4 comes within 35.7 AU from the Sun at perihelion and 47.8 AU at aphelion.[5] It has an orbital inclination of nearly 18° with respect to the ecliptic.[5] 2002 MS4 last passed perihelion in April 1853, passed aphelion in February 1987, and will make its next perihelion passage in June 2123.[23][24][6]

2002 MS4 is located in the classical region of the Kuiper belt 37–48 AU from the Sun,[25]: 227  and is thus classified as a classical Kuiper belt object or cubewano.[3]: 53  2002 MS4's high orbital inclination qualifies it as a dynamically "hot" member of the classical Kuiper belt, which implies that it was gravitationally scattered out to its present location by Neptune's outward planetary migration in the Solar System's early history.[25]: 227, 229  2002 MS4's present orbit is far enough from Neptune (minimum orbit intersection distance 6.6 AU)[1] that it no longer experiences scattering from close encounters with the planet.[4][25]: 214 

A dynamical study in 2007 simulated 2002 MS4's orbital evolution over a 10-million-year timespan and found that it may be in an intermittent 18:11 mean-motion orbital resonance with Neptune,[25]: 218  which seems to cause irregular fluctations in 2002 MS4's orbital inclination and eccentricity.[25]: 225  Despite this, researchers do not consider 2002 MS4 to be in resonance with Neptune.[4][3]: 56 [10]: 2 

 
The 18:11-resonant libration of 2002 MS4's nominal orbit, in a frame co-rotating with Neptune
 
Top and side views of 2002 MS4's orbit (white) with Pluto and other classical Kuiper belt objects for comparison

Observability

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2002 MS4's position in the constellation Scutum in 2020, moving eastward (left) across the brightest areas of the Milky Way

In the night sky, 2002 MS4 is located near the Milky Way's Galactic Center in the southern celestial hemisphere. It has been passing through that region's dense field of background stars since its discovery.[10]: 9  Combined with 2002 MS4's faint apparent magnitude of 20.5 as seen from Earth,[13] its crowded location can make observations difficult.[9]: 92 [10]: 9  On the other hand, 2002 MS4's location makes it viable for observing stellar occultations as there are numerous stars for it to pass in front of.[10]: 9 

Occultations

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2002 MS4 occultations observed in 2019–2022[7]: 5, 18B.4 
Date Star apparent
magnitude
(V-band)		 Positive
detections		 Negative
detections[c]		 Number of
telescope
locations[d]		 Continents
observed
09 Jul 2019 15.00 2 4 10 South America
26 Jul 2019 17.78 3 0 3 South America
26 Jul 2019 15.45 1 0 1 North America
19 Aug 2019 16.51 2 0 2 North America
26 Jul 2020 14.76 2 0 5 Africa
8 Aug 2020 14.62 61 40 116 Europe, Africa, Asia
24 Feb 2021 16.51 1 1 2 South America
14 Oct 2021 15.83 2 0 14 North America
10 Jun 2022 15.1 3 0 3 North America, Africa

Stellar occultations by 2002 MS4 occur when it passes in front of a star and blocks out its light, causing the star to dim for several seconds until 2002 MS4 emerges.[7]: 2  Observing stellar occultations by 2002 MS4 can provide precise measurements for its position, shape, and size.[7]: 1 [8]: 35  Due to parallax between Earth, 2002 MS4, and the occulted star, occultations by 2002 MS4 may only be observable to certain locations on Earth. For this reason, 2002 MS4's orbital trajectory and ephemeris must be precisely known before occultation predictions can be reliably made.[7]: 2 [8]: 35 

To facilitate occultation predictions for 2002 MS4, astronomers of the European Research Council's Lucky Star project gathered astrometric observations of 2002 MS4 from 2009–2019 to reduce its orbital uncertainty and utilized the Gaia catalogues for high-precision positions of stars.[26][7]: 2  From 2019–2022, the Lucky Star project organized campaigns for astronomers worldwide to observe the predicted occultations by 2002 MS4, yielding nine successfully-observed occultations by the end of the period.[7]: 1, 3  The first successfully-observed occultation by 2002 MS4 took place in South America on 9 July 2019, which yielded two positive detections and four negative detections from the 10 participating telescope locations; the remaining four telescopes were affected by poor weather.[26][7]: 2, 18B.4  More successful observations of 2002 MS4's occultations took place on 26 July and 19 August 2019, which provided highly precise astrometry that helped refine later occultation predictions.[27][7]: 2 

On 8 August 2020, the Lucky Star project organized a large observing campaign for 2002 MS4, which would occult a relatively bright star of apparent magnitude 14.6 and be observable over densely-populated regions in multiple continents.[7]: 4  A total of 116 telescope locations from Europe, North Africa, and Western Asia participated in the campaign and yielded 61 positive detections and 40 negative detections, with the remaining 15 telescopes inhibited by poor weather or technical difficulties.[7]: 4, 18B.1–3  The observers of the occultation found no evidence of rings, cometary jets, or natural satellites around 2002 MS4.[7]: 9  This is the most extensive participation in a TNO occultation campaign as of 2023.[28]: 1347 [7]: 9  Thanks to the large amount of positive detections across various locations, the global shape outline and topography of 2002 MS4 could be seen clearly for the first time.[29][7]

  •  
    Map showing the location of telescopes that participated in the 8 August 2020 occultation campaign. Telescopes within the path of 2002 MS4's shadow (region between the two solid blue curves) made positive detections (blue and red points), whereas telescopes outside the path made negative detections (green points).
  •  
    2002 MS4's projected shape revealed by the many positive detection chords from the 8 August 2020 occultation (blue with red error bars). A massive topographic peak and depression is visible along 2002 MS4's limb in the northeast direction.

Physical characteristics

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History of diameter estimates for 2002 MS4
Year of
Publication		 Diameter
(km)		 Method Refs
2008 726.2+123.2
−122.9 		thermal
(Spitzer) 		[30]: 173 
2009 730+118
−120 		thermal
(Spitzer, remodeled) 		[31]: 291 
2012 934±47 thermal
(Herschel) 		[32]: 10 
2020 770±2 occultation
(9 Jul 2019) 		[26]
2022 <810±70 occultation
(26 Jul 2019) 		[33]
2023 796±24 occultation
(8 Aug 2020) 		[7][e]

Results from the extensively observed 8 August 2020 occultation show that 2002 MS4 has a shape close to that of an oblate spheroid, with an equatorial diameter of 814 km (506 mi) and a polar diameter of up to 770 km (480 mi).[7]: 5  2002 MS4's mean diameter from these dimensions is 796 km (495 mi), which places it between the diameters of the two largest asteroids, Ceres and Vesta.[7]: 5  It is unknown whether 2002 MS4's equator is being viewed obliquely or edge-on from Earth's perspective, so it is possible that the object's actual polar diameter may be smaller, or have a greater oblateness, than observed in the August 2020 occultation.[7]: 8  2002 MS4 is the 10th (or 11th if counting Pluto's moon Charon) largest known TNO. Because of its large size, it is considered a dwarf planet candidate by astronomers.[34]: 245 [7]: 1 [8]: iii  With measurement uncertainties considered, it is tied with 2002 AW197 and 2013 FY27 (diameters 729–807 km[35] and 659–820 km,[36] respectively) as the largest unnamed object in the Solar System.

2002 MS4 was previously thought to have a larger diameter of 934 km (580 mi), according to infrared thermal emission measurements made by the Spitzer and Herschel space telescopes in 2006 and 2010.[32]: 4, 7, 10  This thermal emission-derived diameter disagrees with the occultation-derived diameter; if both the thermal emission measurements and occultation-derived diameter are correct, then 2002 MS4 would be emitting more thermal radiation than predicted if it were a non-rotating, simple airless body.[8]: 68, 70, 73  It is not yet clear why 2002 MS4 seems to be emitting excess thermal radiation; it could be possible that either there is an unknown satellite of 2002 MS4 contributing to the excess thermal emission,[7]: 9  or the predictions for 2002 MS4's thermal emission behavior are inaccurate.[8]: 73 

The mass and density of 2002 MS4 is unknown since it has no known moons; otherwise, estimation of its mass would have been possible by Kepler's third law.[8]: 35  Without a known mass and density, it is not possible to determine whether 2002 MS4's spheroidal shape is due to hydrostatic equilibrium, which would qualify it as a dwarf planet.[37]: 10  Inferring from its diameter and albedo, 2002 MS4 is probably not in hydrostatic equilibrium since it lies within the 400–1,000 km (250–620 mi) diameter range where TNOs are typically observed with very low densities, presumably due to having highly porous interior structures that have not gravitationally compressed into solid bodies.[38]: 1, 8  Otherwise, if 2002 MS4 is in hydrostatic equilibrium, then its density could be estimated from its oblateness and rotation period.[7]: 8  However, both of these properties are poorly known for 2002 MS4, so only its minimum and maximum possible densities could be estimated.[7]: 8  Assuming a Maclaurin spheroid as the equilibrium shape for 2002 MS4, the ranges of possible densities are 0.72–8.0 g/cm3 and 0.36–3.9 g/cm3 for possible rotation periods of 7.44 and 10.44 hours, respectively.[7]: 8 

Surface

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2002 MS4 has a gray or spectrally neutral surface color, meaning it reflects similar amounts of light for wavelengths across the visible spectrum.[12]: 6  In Barucci et al.'s classification scheme for TNO color indices, 2002 MS4 falls under the BB group of TNOs with neutral colors, whose surface compositions characteristically have a high fraction of water ice and amorphous carbon but low amounts of tholins.[39]: 1294, 1296  Near-infrared spectroscopy by the James Webb Space Telescope (JWST) in 2022 revealed the presence of crystalline water ice, amorphous water ice, and carbon dioxide ice in 2002 MS4's surface.[40][11] The large Kuiper belt object 120347 Salacia was observed by JWST to have a similar surface composition as 2002 MS4.[11] Preliminary modeling of 2002 MS4's JWST spectrum by Cook et al. suggests that the water ice on the object's surface consists of micrometer-sized grains and the carbon dioxide ice consists of a mix of coarser, micrometer-sized grains to finer, sub-micrometer-sized grains.[11] Tholins should also exist on 2002 MS4's surface according to Cook et al.'s preliminary model, although they have not been detected in 2002 MS4's JWST spectrum.[11] Volatile ices such as methane were also not detected in 2002 MS4's JWST spectrum.[40] The lack of volatiles on 2002 MS4's surface agrees with its low geometric albedo of 0.1 determined from observations by the New Horizons spacecraft, which indicates 2002 MS4 has a very dark and unevolved surface in contrast to the bright and volatile-rich dwarf planets like Pluto.[10]: 2, 18–19  New Horizons observations of 2002 MS4's phase curve indicate that the icy regolith grains on the object's surface are rough and irregularly shaped.[10]: 19 

Topographic features

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Projected shape of 2002 MS4 seen in the 8 August 2020 occultation
 
Plot of topographic elevation variations along 2002 MS4's limb

The 8 August 2020 occultation revealed massive topographic features along 2002 MS4's northeastern outline, or limb, which notably includes a crater-like depression 322 ± 39 km (200 ± 24 mi) wide and 45.1 ± 1.5 km (28.02 ± 0.93 mi) deep, and a 25+4
−5 km (15.5+2.5
−3.1 mi)-tall peak near the rim of the depression.[7]: 7  Another depression feature about 10 km (6.2 mi) wide and 11 km (6.8 mi) deep was detected by a single telescope from Varages, France during the occultation; this depression feature partially occulted the star as 2002 MS4 emerged, which resulted in the star brightening gradually instead of instantly.[7]: 7  The elevations of these observed topographic features lie beyond the maximum elevation of 6–7 km (3.7–4.3 mi) expected for an icy body of 2002 MS4's size, signifying that the object may have experienced a large impact in its past.[7]: 6, 9  It would be possible for 2002 MS4 to support its massive topographic features if its material strength increases toward its core.[7]: 6  Topographic features on other TNOs have been previously observed through occultation, such as (208996) 2003 AZ84 which has a depression feature at least 8 km (5 mi) deep.[41][42]

The topographic peak on 2002 MS4 has a height comparable to Mars's tallest mountain, Olympus Mons, and the central mound of the Rheasilvia crater on asteroid Vesta.[42][43] If 2002 MS4's topographic peak is a mountain, then it would qualify as one of the tallest known mountains in the Solar System.[42] It is possible that this topographic peak may actually be an unknown 213 km (132 mi)-diameter satellite that was passing in front or behind 2002 MS4 during the occultation, but this scenario is unlikely according to Bruno Sicardy, one of the occultation team members.[7]: 9, 25 [42] A satellite of this size would not be large enough to explain 2002 MS4's excess thermal emission.[7]: 25 

If 2002 MS4's massive depression is a crater, then it would be the first observation of a massive crater on a TNO.[7]: 9  The depression's width takes up about 40% of 2002 MS4's diameter, which is comparable to the largest crater-to-diameter ratios seen in Saturn's moons Tethys and Iapetus. For context, Tethys's largest crater Odysseus takes up about 43% of its diameter, while Iapetus's largest crater Turgis takes up about 40% of its diameter, but they are much shallower than the purported 2002 MS4 crater.[7]: 9  The trans-Neptunian dwarf planets Pluto and Charon do not exhibit such large craters on the other hand,[f] as their largest crater-to-diameter ratios are 10.5% and 18.9%, respectively.[7]: 9  The depth of 2002 MS4's massive depression takes up 5.7% of 2002 MS4's diameter and exceeds those seen in the largest craters of other Solar System bodies of comparable size: the largest crater of Saturn's moon Mimas has a depth of up to 10–12 km (6.2–7.5 mi)[44]: 424  and Vesta's Rheasilvia crater has a depth of up to 25 km (16 mi).[43]

Rotation and light curve

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The rotation period of 2002 MS4 is uncertain and its rotational axial tilt is unknown. It is difficult to measure 2002 MS4's rotation period photometrically with telescopes on Earth since the object is obscured in a dense field of background stars.[9]: 118 [7]: 7  Due to 2002 MS4's spheroidal shape and possible surface albedo variations, its light curve only exhibits very small fluctuations in brightness (amplitude 0.05–0.12 mag[8]: 85 ) over time as it rotates.[7]: 7 [8]: 73  The first attempts at measuring 2002 MS4's rotation were made with the Sierra Nevada Observatory's 1.5-meter telescope in August 2005, but it did not observe the object long enough to identify any periodicities in its light curve.[9]: 31, 92  Subsequent observations by the Galileo National Telescope in June–July 2011 took advantage of 2002 MS4 passing in front of a dark nebula, which enabled it to determine possible periods of either 7.33 hours or 10.44 hours.[9]: 94  On the other hand, observations by the Canada–France–Hawaii Telescope in July–August 2013 measured a rotation period of 14.251 hours, with other less probable rotation period aliases of 8.932 and 5.881 hours.[8]: 43, 53, 74 

Exploration

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New Horizons

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The New Horizons spacecraft observed 2002 MS4 during 2016–2019, as part of its extended Kuiper belt mission after its successful Pluto flyby in 2015.[10]: 8  2002 MS4 was 15.3 AU (2.29 billion km; 1.42 billion mi) away from the spacecraft when it began observations on 13 July 2016, and was 12.0 AU (1.80 billion km; 1.12 billion mi) away from the spacecraft when it ended observations in 1 September 2019.[10]: 8  New Horizons had the unique vantage point of observing 2002 MS4 and other TNOs while it was inside the Kuiper belt, which allowed the spacecraft to observe these objects at high phase angles (>2°) that are not observable from Earth.[10]: 1  By observing how 2002 MS4's brightness changes as a function of phase angle, the object's phase curve could be determined, which can reveal the light scattering properties of 2002 MS4's surface regolith.[10]: 1  In addition to significantly improving the knowledge of 2002 MS4's phase curve, the observations by New Horizons also significantly improved the precision of 2002 MS4's orbit.[45]

  •  
    2002 MS4 imaged by the New Horizons spacecraft in July 2016, from a distance of 15.3 AU (2.3 billion km; 1.4 billion mi)
  •  
    New Horizons trajectory through the Kuiper belt, with positions of nearby KBOs including 2002 MS4 labeled

Proposed

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2002 MS4 has been considered as a possible exploration target for future missions to the Kuiper belt and beyond, such as NASA's Interstellar Probe concept.[46] A 2019 study by Amanda Zangari and collaborators identified several possible trajectories to 2002 MS4 for a spacecraft that would be launched in 2025–2040.[47] For a spacecraft launched in 2027–2031, a single gravity assist from Jupiter could bring a spacecraft to 2002 MS4 over a minimum duration of 9.1–12.8 years, depending on the excess launch energy of the spacecraft.[47]: 922  Another trajectory using a single Jupiter gravity assist for a 2040 launch date could bring a spacecraft to 2002 MS4 over a minimum duration of 13 years.[47]: 922  A 2038–2040 launch trajectory using a single Saturn gravity assist could bring a spacecraft to 2002 MS4 over a minimum duration of 16.7 years,[47]: 925  while a 2038–2040 launch trajectory using two gravity assists from Jupiter and Saturn could bring a spacecraft to 2002 MS4 over a minimum duration of 18.6–19.5 years.[47]: 923 

See also

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Notes

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  1. ^ The "single-peaked" rotation period refers to the peak-to-trough period in 2002 MS4's light curve. The single-peaked period is the true rotation period of 2002 MS4 if the object is spheroidal and has albedo variations on its surface. If 2002 MS4 is an elongated triaxial ellipsoid on the other hand, then it would produce a double-peaked light curve, where the object's true rotation period is double the single-peaked period since it spans two peaks and two troughs in its light curve.[9]: 77 
  2. ^ These orbital elements are expressed in terms of the Solar System Barycenter (SSB) as the frame of reference.[5] Due to planetary perturbations, the Sun revolves around the SSB at non-negligible distances, so heliocentric-frame orbital elements and distances can vary in short timescales as shown in JPL-Horizons.[22]
  3. ^ Telescopes that were affected by poor weather or technical problems are not counted as negative detections.
  4. ^ Telescopes that are located in the same place or are located very close together are considered single locations.
  5. ^ Rommel et al. previously reported a diameter of 800±24 km in a 2021 conference talk about their preliminary 8 August 2020 occultation results.[29] This preliminary diameter estimate has been superseded by the more recent estimate of 796±24 km in their paper published in 2023.[7]
  6. ^ Pluto has an over-1,000 km (620 mi)-wide ice-covered basin named Sputnik Planitia, although it is unclear whether it originated from an impact.

References

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  1. ^ a b c d e f g "(307261) = 2002 MS4". Minor Planet Center. Retrieved 13 September 2021.
  2. ^ a b c d e "JPL Small-Body Database Lookup: 307261 (2002 MS4)" (2022-07-04 last obs.). Jet Propulsion Laboratory. Retrieved 10 December 2023.
  3. ^ a b c d Gladman, Brett; Marsden, Brian G.; VanLaerhoven, Christa (2008). "Nomenclature in the Outer Solar System" (PDF). The Solar System Beyond Neptune. University of Arizona Press. pp. 43–57. arXiv:astro-ph/0702538. Bibcode:2008ssbn.book...43G. ISBN 9780816527557. S2CID 14469199.
  4. ^ a b c Buie, Marc W. "Orbit Fit and Astrometric record for 307261". Southwest Research Institute. Archived from the original on 27 June 2021. Retrieved 13 September 2021.
  5. ^ a b c d e f "JPL Horizons On-Line Ephemeris for 307261 (2002 MS4) at epoch JD 2460000.5". JPL Horizons On-Line Ephemeris System. Jet Propulsion Laboratory. Retrieved 19 June 2022. Solution using the Solar System Barycenter. Ephemeris Type: Elements and Center: @0)
  6. ^ a b "JPL Horizons On-Line Ephemeris for 307261 (2002 MS4) from 2123-Jan-01 to 2124-Jan-01". JPL Horizons On-Line Ephemeris System. Jet Propulsion Laboratory. Retrieved 28 June 2022. (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 1-sigma from JPL Small-Body Database.)
  7. ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak al am Rommel, F. L.; Braga-Ribas, F.; Ortiz, J. L.; Sicardy, B.; Santos-Sanz, P.; Desmars, J.; et al. (October 2023). "A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations". Astronomy & Astrophysics. 678: 25. arXiv:2308.08062. Bibcode:2023A&A...678A.167R. doi:10.1051/0004-6361/202346892. S2CID 260926329. A167.
  8. ^ a b c d e f g h i j k Peng, Jinghan (September 2023). Phase Dependent Variation in the Reflectivity of Kuiper Belt Object 2002 MS4 (PDF) (MSc thesis). University of Victoria. hdl:1828/15363. Archived (PDF) from the original on 9 September 2023. Retrieved 9 September 2023.
  9. ^ a b c d e f Thirouin, Audrey (2013). Study of Trans-Neptunian Objects using photometric techniques and numerical simulations (PDF) (PhD thesis). University of Granada. Bibcode:2013PhDT.......246T. S2CID 125259956. Archived (PDF) from the original on 19 December 2019. Retrieved 19 November 2013.
  10. ^ a b c d e f g h i j k l Verbiscer, Anne J.; Helfenstein, Paul; Porter, Simon B.; Benecchi, Susan D.; Kavelaars, J. J.; Lauer, Tod R.; et al. (April 2022). "The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons". The Planetary Science Journal. 3 (4): 31. Bibcode:2022PSJ.....3...95V. doi:10.3847/PSJ/ac63a6. 95.
  11. ^ a b c d e Cook, J. C.; Brunetto, R.; De Souza Feliciano, A. C.; Emery, J.; Holler, B.; Parker, A. H.; et al. (June 2023). Hapke Modeling of Several KBOs from JWST Observations (ePoster) (PDF). Asteroids, Comets, Meteors Conference 2023. Lunar and Planetary Institute. Archived (PDF) from the original on 10 December 2023.
  12. ^ a b Tegler, S. C.; Romanishin, W.; Consolmagno, G. J. (December 2016). "Two Color Populations of Kuiper Belt and Centaur Objects and the Smaller Orbital Inclinations of Red Centaur Objects". The Astronomical Journal. 152 (6): 13. Bibcode:2016AJ....152..210T. doi:10.3847/0004-6256/152/6/210. S2CID 125183388. 210.
  13. ^ a b "(307261) 2002MS4 Ephemerides". Asteroids Dynamic Site. Department of Mathematics, University of Pisa, Italy. Retrieved 19 November 2019.
  14. ^ a b c Trujillo, C. A.; Brown, M. E. (June 2003). "The Caltech Wide Area Sky Survey". Earth, Moon, and Planets. 92 (1): 99–112. Bibcode:2003EM&P...92...99T. doi:10.1023/B:MOON.0000031929.19729.a1. S2CID 189905639.
  15. ^ Schilling, Govert (2008). The Hunt For Planet X. Springer. p. 214. ISBN 978-0-387-77804-4.
  16. ^ a b Trujillo, C. A.; Brown, M. E.; Helin, E. F.; Pravdo, S.; Lawrence, K.; Hicks, M.; Nash, C.; Jordan, A. B.; Staples, S.; Schwartz, M.; Marsden, B. G. (21 November 2002). "MPEC 2002-W27 : 2002 MS4, 2002 QX47, 2002 VR128". Minor Planet Electronic Circular. 2002-W27. Minor Planet Center. Bibcode:2002MPEC....W...27T. Retrieved 26 August 2009.
  17. ^ "MPEC 2003-M44 : 2002 KW14, 2002 MS4". Minor Planet Electronic Circular. Minor Planet Center. 29 May 2003. Retrieved 20 June 2022.
  18. ^ a b c Lowe, Andrew. "(307261) 2002 MS4 Precovery Images". andrew-lowe.ca. Retrieved 20 June 2022.
  19. ^ "M.P.S. 231732" (PDF). Minor Planet Circulars Supplement (231732). Minor Planet Center: 42. 30 December 2007. Retrieved 19 November 2019.
  20. ^ "M.P.C. 77416" (PDF). Minor Planet Circulars (77416). Minor Planet Center: 292. 10 December 2011. Retrieved 20 June 2022.
  21. ^ a b "Rules and Guidelines for Naming Non-Cometary Small Solar-System Bodies" (PDF). IAU Working Group for Small Bodies Nomenclature. 20 December 2021. p. 10. Retrieved 20 June 2022.
  22. ^ "JPL Horizons On-Line Ephemeris for 307261 (2002 MS4) at epochs JD 2450000.5–2460000.5". JPL Horizons On-Line Ephemeris System. Jet Propulsion Laboratory. Retrieved 28 June 2022. Solution using the Sun. Ephemeris Type: Elements and Center: @sun)
  23. ^ "JPL Horizons On-Line Ephemeris for 307261 (2002 MS4) from 1853-Jan-01 to 1854-Jan-01". JPL Horizons On-Line Ephemeris System. Jet Propulsion Laboratory. Retrieved 28 June 2022. (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 1-sigma from JPL Small-Body Database.)
  24. ^ "JPL Horizons On-Line Ephemeris for 307261 (2002 MS4) from 1987-Jan-01 to 1988-Jan-01". JPL Horizons On-Line Ephemeris System. Jet Propulsion Laboratory. Retrieved 10 December 2022. (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 1-sigma from JPL Small-Body Database.)
  25. ^ a b c d e Lykawka, Patryk Sofia; Tadashi, Mukai (July 2007). "Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation". Icarus. 189 (1): 213–232. Bibcode:2007Icar..189..213L. doi:10.1016/j.icarus.2007.01.001. S2CID 122671996.
  26. ^ a b c Rommel, Flavia Luane; Braga-Ribas, Felipe; Pereira, Crystian Luciano; Desmars, Josselin; Santos-Sanz, Pablo; Benedetti-Rossi Rossi, Gustavo; et al. (September 2020). Results on stellar occultations by (307261) 2002 MS4. 14th Europlanet Science Congress 2020. Europlanet Society. Bibcode:2020EPSC...14..866L. doi:10.5194/epsc2020-866. EPSC2020-866. Retrieved 6 September 2021.
  27. ^ "2002 MS4 08/08/2020". ERC Lucky Star project. Retrieved 6 September 2021.
  28. ^ Kilic, Y.; Braga-Ribas, F.; Kaplan, M.; Erece, O.; Souami, D.; Dindar, M.; et al. (September 2022). "Occultation portal: A web-based platform for data collection and analysis of stellar occultations". Monthly Notices of the Royal Astronomical Society. 515 (1): 1346–1357. arXiv:2206.09615. Bibcode:2022MNRAS.515.1346K. doi:10.1093/mnras/stac1595.
  29. ^ a b Rommel, Flavia L.; Braga-Ribas, Felipe; Vara-Lubiano, Mónica; Ortiz, Jose L.; Desmars, Josselin; Morgado, Bruno E.; et al. (September 2021). Evidence of topographic features on (307261) 2002 MS4 surface. 15th Europlanet Science Congress 2021. Europlanet Society. Bibcode:2021EPSC...15..440R. doi:10.5194/epsc2021-440. EPSC2021-440. Retrieved 13 September 2021.
  30. ^ Stansberry, John; Grundy, Will; Brown, Mike; Cruikshank, Dale; Spencer, John; Trilling, David; Margot, Jean-Luc (2008). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from the Spitzer Space Telescope" (PDF). The Solar System Beyond Neptune. University of Arizona Press. pp. 161–179. arXiv:astro-ph/0702538. Bibcode:2008ssbn.book..161S. ISBN 9780816527557. S2CID 578439.
  31. ^ Brucker, M. J.; Grundy, W. M.; Stansberry, J. A.; Spencer, J. R.; Sheppard, S. S.; Chiang, E. I.; Buie, M. W. (May 2009). "High albedos of low inclination Classical Kuiper belt objects". Icarus. 201 (1): 284–294. arXiv:0812.4290. Bibcode:2009Icar..201..284B. doi:10.1016/j.icarus.2008.12.040. S2CID 53543791.
  32. ^ a b Vilenius, E.; Kiss, C.; Mommert, M.; Müller, T.; Santos-Sanz, P.; Pal, A.; et al. (May 2012). ""TNOs are Cool": A survey of the trans-Neptunian region VI. Herschel/PACS observations and thermal modeling of 19 classical Kuiper belt objects" (PDF). Astronomy & Astrophysics. 541: 17. arXiv:1204.0697. Bibcode:2012A&A...541A..94V. doi:10.1051/0004-6361/201118743. S2CID 54222700. A94.
  33. ^ Zemouri, Rami; Ceravolo, Peter; Kavelaars, JJ; Bridges, Terry (March 2022). "Report on Three Stellar Occultations by the Excited Kuiper Belt Object 2002 MS4". Research Notes of the AAS. 6 (3). Bibcode:2022RNAAS...6...59Z. doi:10.3847/2515-5172/ac5f3b. 59.
  34. ^ Pinilla-Alonso, Noemi (August 2015). "Icy Dwarf Planets: Colored Popsicles in the Outer Solar System". Proceedings of the International Astronomical Union. 11: 241–246. Bibcode:2016IAUFM..29A.241P. doi:10.1017/S1743921316002970. A29A.
  35. ^ Vilenius, E.; Kiss, C.; Müller, T.; Mommert, M.; Santos-Sanz, P.; Pál, A.; et al. (April 2014). ""TNOs are Cool": A survey of the trans-Neptunian region. X. Analysis of classical Kuiper belt objects from Herschel and Spitzer observations". Astronomy & Astrophysics. 564: 18. arXiv:1403.6309. Bibcode:2014A&A...564A..35V. doi:10.1051/0004-6361/201322416. S2CID 118513049. A35.
  36. ^ Sheppard, Scott S.; Fernandez, Yanga F.; Moullet, Arielle (December 2018). "The Albedos, Sizes, Colors, and Satellites of Dwarf Planets Compared with Newly Measured Dwarf Planet 2013 FY27". The Astronomical Journal. 156 (6): 11. arXiv:1809.02184. Bibcode:2018AJ....156..270S. doi:10.3847/1538-3881/aae92a. S2CID 119522310. 270.
  37. ^ Lineweaver, Charles H.; Norman, Marc (28–30 September 2009). Short, W.; Cairns, I. (eds.). The Potato Radius: a Lower Minimum Size for Dwarf Planets (PDF). Proceedings of the 9th Australian Space Science Conference. National Space Society of Australia (published 2010). pp. 67–78. arXiv:1004.1091. Bibcode:2010arXiv1004.1091L. ISBN 9780977574032.
  38. ^ Grundy, W. M.; Noll, K. S.; Buie, M. W.; Benecchi, S. D.; Ragozzine, D.; Roe, H. G. (December 2019). "The Mutual Orbit, Mass, and Density of Transneptunian Binary Gǃkúnǁʼhòmdímà ((229762) 2007 UK126)" (PDF). Icarus. 334: 30–38. Bibcode:2019Icar..334...30G. doi:10.1016/j.icarus.2018.12.037. S2CID 126574999.
  39. ^ Barucci, M. A.; Belskaya, I.; Fulchignoni, M.; Birlan, M. (September 2005). "Taxonomy of Centaurs and Trans-Neptunian Objects". The Astronomical Journal. 130 (3): 1291–1298. Bibcode:2005AJ....130.1291B. doi:10.1086/431957. S2CID 32008426.
  40. ^ a b Cook, J. C.; Brunetto, R.; De Souza Feliciano, A. C.; Emery, J.; Holler, B.; Parker, A. H.; et al. (June 2023). Hapke Modeling of Several KBOs from JWST Observations (PDF). Asteroids, Comets, Meteors Conference 2023. Lunar and Planetary Institute. Archived (PDF) from the original on 10 December 2023.
  41. ^ Dias-Oliveira, A.; Sicardy, B.; Ortiz, J. L.; Braga-Ribas, F.; Leiva, R.; Vieira-Martins, R.; et al. (July 2017). "Study of the Plutino Object (208996) 2003 AZ84 from Stellar Occultations: Size, Shape, and Topographic Features". The Astronomical Journal. 154 (1): 13. arXiv:1705.10895. Bibcode:2017AJ....154...22D. doi:10.3847/1538-3881/aa74e9. S2CID 119098862. 22.
  42. ^ a b c d O'Callaghan, Jonathan (29 August 2023). "Massive crater found on distant world far beyond Neptune". New Scientist. Retrieved 17 September 2023.
  43. ^ a b Schenk, P.; Marchi, S.; O'Brien, D. P.; Buczkowski, D. L.; Jaumann, R.; Yingst, A.; et al. (March 2012). Mega-Impacts into Planetary Bodies: Global Effects of the Giant Rheasilvia Impact Basin on Vesta (PDF). 43rd Lunar and Planetary Science Conference. Lunar and Planetary Institute. Archived (PDF) from the original on 22 October 2015.
  44. ^ Moore, Jeffery M.; Schenk, Paul M.; Bruesch, Lindsey S.; Asphaug, Erik; McKinnon, William B. (May 2004). "Large impact features on middle-sized icy satellites". Icarus. 171 (2): 421–443. Bibcode:2004Icar..171..421M. doi:10.1016/j.icarus.2004.05.009. S2CID 35696739.
  45. ^ Lakdawalla, Emily (24 January 2018). "New Horizons prepares for encounter with 2014 MU69". The Planetary Society. Retrieved 13 November 2019.
  46. ^ Runyon, Kirby; Holler, Bryan; Bannister, Michele (September 2020). Exploring Trans-Neptunian Objects with Interstellar Probe. 14th Europlanet Science Congress 2020. Europlanet Society. Bibcode:2020EPSC...14..276R. doi:10.5194/epsc2020-276. EPSC2020-276. Retrieved 10 December 2023.
  47. ^ a b c d e Zangari, Amanda M.; Finley, Tiffany J.; Stern, S. Alan; Tapley, Mark B. (May 2019). "Return to the Kuiper Belt: Launch Opportunities from 2025 to 2040". Journal of Spacecraft and Rockets. 56 (3): 919–930. arXiv:1810.07811. Bibcode:2019JSpRo..56..919Z. doi:10.2514/1.A34329. S2CID 119033012.
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