Sedna (dwarf planet)

Template:Short description Template:Featured article Template:Use American English Template:Use dmy dates {{#invoke:infobox|infoboxTemplate | class = vcard | titleclass = fn org | title = 90377 Sedna | image = {{#invoke:InfoboxImage|InfoboxImage|image=Sedna PRC2004-14d.jpg|upright={{#if:||1.1}}|alt=Single fuzzy white dot with lots of background noise}} | caption = Low-resolution image of Sedna by the Hubble Space Telescope, March 2004 | headerstyle = {{#if:#C2E0FF|background-color:#C2E0FF|background-color:#E0CCFF}} | labelstyle = max-width:{{#if:||11em}}; | autoheaders = y

| header1 = Discovery<ref name="discovery" />

| header10 = {{#if:|Designations|Designations}}

| header20 = Orbital characteristics{{#ifeq:yes|yes| (barycentric)}}<ref name="jpldata" />

| data21 = | data22 = {{#if:31 May 2020 (JD 2458900.5) |Epoch 31 May 2020 (JD 2458900.5)}} | data23 = {{#if:2 | Uncertainty parameter 2}} | label24 = Observation arc | data24 = 30 years | label25 = Earliest precovery date | data25 = 25 September 1990 | label26 = {{#switch:{{{apsis}}} |apsis|gee|barion|center|centre|(apsis)=Apo{{{apsis}}} |Ap{{#if:|{{{apsis}}}|helion}}}} | data26 = Template:Convert<ref name="barycenter"/><ref group=lower-alpha name=footnoteG/> | label27 = Peri{{#if:|{{{apsis}}}|helion}} | data27 = Template:Convert<ref name="Perihelion2076"/><ref name="barycenter"/><ref name="AstDyS2076" /> | label28 = Peri{{#if:|{{{apsis}}}|apsis}} | data28 = | label29 = {{#switch:{{{apsis}}} |helion|astron=Ap{{{apsis}}} |Apo{{#if:|{{{apsis}}}|apsis}}}} | data29 = | label30 = Periastron | data30 = | label31 = Apoastron | data31 = | label32 = Template:Longitem | data32 = Template:Convert<ref name="barycenter"/> or 0.007 ly | label33 = Template:Longitem | data33 = | label34 = Eccentricity | data34 = 0.8496<ref name="barycenter"/> | label35 = Template:Longitem | data35 = Template:Val yr (barycentric)<ref group=lower-alpha name=footnoteG/> | label36 = Template:Longitem | data36 = 11,408 Gregorian years | label37 = Template:Longitem | data37 = 1.04 km/s | label38 = Template:Longitem | data38 = 358.117° | label39 = Template:Longitem | data39 = Template:Deg2DMS / day | label40 = Inclination | data40 = 11.9307° | label41 = Template:Longitem | data41 = | label42 = Template:Longitem | data42 = 144.248° | label43 = Template:Longitem | data43 = | label44 = Template:Longitem | data44 = ≈ 18 July 2076<ref name="Perihelion2076"/><ref name="AstDyS2076" /> | label45 = Template:Longitem | data45 = 311.352° | label46 = Template:Nowrap | data46 = | label47 = Satellite of | data47 = | label48 = Group | data48 = | label49 = {{#switch: |yes|true=Satellites |Known satellites}} | data49 = | label50 = Star | data50 = | label51 = Earth MOID | data51 = | label52 = Mercury MOID | data52 = | label53 = Venus MOID | data53 = | label54 = Mars MOID | data54 = | label55 = Jupiter MOID | data55 = | label56 = Saturn MOID | data56 = | label57 = Uranus MOID | data57 = | label58 = Neptune MOID | data58 = | label59 = T_Jupiter | data59 =

| header60 = Proper orbital elements

| label61 = Template:Longitem | data61 = {{#if: |{{{p_semimajor}}} AU}} | label62 = Template:Longitem | data62 = | label63 = Template:Longitem | data63 = | label64 = Template:Longitem | data64 = {{#if: |{{{p_mean_motion}}} deg Template:\yr}} | label65 = Template:Longitem | data65 = {{#if:|{{#expr:360/1 round 5}} yr
({{#expr:365.25*360/1 round 3}} d) }} | label66 = Template:Longitem | data66 = {{#if:|{{{perihelion_rate}}} arcsec Template:\yr }} | label67 = Template:Longitem | data67 = {{#if:|{{{node_rate}}} arcsec Template:\yr}}

| header70 = Template:Anchor{{#if:yes| Physical characteristics|Physical characteristics}}

| label71 = Dimensions | data71 = | label72 = Template:Longitem | data72 = Template:Val<ref name="Lellouch A60">Template:Cite journal</ref>
Template:Val
(occultation chord)<ref name="Rommel2020"/> | label73 = Template:Longitem | data73 = | label74 = Template:Longitem | data74 = | label75 = Template:Longitem | data75 = | label76 = Flattening | data76 = | label77 = Circumference | data77 = | label78 = Template:Longitem | data78 = | label79 = Volume | data79 = | label80 = Mass | data80 = | label81 = Template:Longitem | data81 = | label82 = Template:Longitem | data82 = | label83 = Template:Longitem | data83 = | label84 = Template:Longitem | data84 = | label85 = Template:Longitem | data85 = Template:Val h
(~18 h less likely)<ref name="Gaudi2005" /> | label86 = Template:Longitem | data86 = | label87 = Template:Longitem | data87 = | label88 = Template:Longitem | data88 = | label89 = Template:Longitem | data89 = | label90 = Template:Longitem | data90 = | label91 = Template:Longitem | data91 = | label92 = Template:Longitem | data92 = | label93 = {{#if:yes |Template:Longitem |Albedo}} | data93 = Template:Val<ref name="Lellouch A60">Template:Cite journal</ref> | label94 = Temperature | data94 = ≈ 12 K (see note)

| data100 = {{#if:|

Surface temp.	min	mean	max
{{{temp_name1}}}
{{{temp_name2}}}
{{{temp_name3}}}
{{{temp_name4}}}

}}

| header110 = Atmosphere

| below = {{#if:||Template:Reflist }}

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Sedna (minor-planet designation: 90377 Sedna) is a dwarf planet in the outermost reaches of the Solar System, orbiting the Sun far beyond the orbit of Neptune. Discovered in 2003, the frigid planetoid is one of the reddest known among Solar System bodies. Detailed spectroscopic analysis has revealed Sedna's surface to be a mixture of the solid ices of water (H₂O),<ref name=":1">Template:Cite journal</ref> carbon dioxide (CO₂), and ethane (C₂H₆), along with occasional sedimentary deposits of methane (CH₄)-derived,<ref>Template:Cite journal</ref> vividly reddish-colored organic tholins,<ref name=":1" /> a surface chemical makeup somewhat similar to those of other trans-Neptunian objects.<ref>Template:Cite journal</ref> Sedna has no detectable atmosphere, as its temperature is far too low for solids to volatilize.<ref>Template:Cite journal</ref> Within range of uncertainty, it is tied with the dwarf planet Template:Dp in the asteroid belt as the largest dwarf planet not known to have a moon. With a diameter of roughly 1,000 km,<ref>Template:Cite journal</ref> it is nearly the size of Tethys around Saturn. Owing to its lack of known moons,<ref>Template:Cite journal</ref> the Keplerian laws of planetary motion cannot be utilized for determining its mass, and the actual figure remains as yet unknown.

Sedna's orbit is one of the widest known in the Solar System. Its aphelion, the farthest point from the Sun in its orbit, is located 937 astronomical units (AU) away.<ref name="barycenter"/> This is some 19 times that of Pluto, leading to it spending most of its time well beyond the heliopause (120 AU),<ref>Template:Cite journal</ref> the boundary beyond which the influences of particles from interstellar space dominate those from the Sun. Sedna's orbit is also one of the most elliptical and narrow discovered, with an eccentricity of 0.8496. This implies that its perihelion, or point of closest approach to the Sun, at 76 AU is around 12.3 times as close as its aphelion. Template:As of, Sedna is Template:Convert from the Sun,<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> approaching perihelion at ~4.4 km/s,<ref>Conservation of specific kinetic + potential energy, with Sun's gravitational parameter substituted.

<math>\frac{1.327 \cdot 10^{20}}{1.495 \cdot 10^{8}} \, \left(\frac{1}{83.2} - \frac{1}{937}\right) = \frac{1}{2} \, \left(x^{2} - 377^{2}\right)</math></ref> and 2.5 times as far away as Neptune. The dwarf planets Template:Dp and Template:Dp are presently farther away from the Sun. A transfer window for a probe fly-by in 2029 utilizing a gravitational assist from Jupiter was proposed, taking 25 years to travel to the dwarf planet, 80 AU (12 billion kilometers) distant.<ref>Template:Cite journal</ref>

Due to its exceptionally elongated orbit, the dwarf planet takes approximately 11,400 years to return to the same point in its orbit around the Sun. The International Astronomical Union (IAU) initially classified Sedna as a member of the scattered disc, a group of objects sent into high-eccentricity orbits by the gravitational influence of Neptune. However, several astronomers who worked in the associated field contested this classification as even its perihelion is far too distant for it to have been scattered by any of the currently known planets. This has led some astronomers to informally refer to it as the first known member of the inner Oort cloud. The dwarf planet is also the prototype of a new orbit class of objects named after itself, the sednoids, which include Template:Mpl and Leleākūhonua, both celestial bodies with large perihelion distances and high eccentricities.<ref>Template:Cite journal</ref>

The astronomer Michael E. Brown, co-discoverer of Sedna, has argued that its unusual orbit could provide information on the early evolution of the Solar System.<ref name="fussman"/><ref name=Chang_2016/> Sedna might have been perturbed into its orbit by a star within the Sun's birth cluster, or captured from a nearby wandering star, or have been sent into its present orbit through a close gravitational encounter with the hypothetical 9th planet, sometime during the solar system's formation.<ref>Template:Cite journal</ref> The statistically unusual clustering to one side of the solar system of the aphelions of Sedna and other similar objects is speculated to be the evidence for the existence of a planet beyond the orbit of Neptune,<ref>Template:Cite journal</ref> which would by itself orbit on the opposing side of the Sun.<ref name="Mike"/><ref name=Lakdawalla_2014/><ref name="Evidence for a Distant Giant Planet"/>

HistoryEdit

DiscoveryEdit

Sedna (provisionally designated Template:Mp) was discovered by Michael Brown (Caltech), Chad Trujillo (Gemini Observatory), and David Rabinowitz (Yale University) on 14 November 2003. The discovery formed part of a survey begun in 2001 with the Samuel Oschin telescope at Palomar Observatory near San Diego, California, using Yale's 160-megapixel Palomar Quest camera. On that day, an object was observed to move by 4.6 arcseconds over 3.1 hours relative to stars, which indicated that its distance was about 100 AU. Follow-up observations were made in November–December 2003 with the SMARTS (Small and Medium Research Telescope System) at Cerro Tololo Inter-American Observatory in Chile, the Tenagra IV telescope in Nogales, Arizona, and the Keck Observatory on Mauna Kea in Hawaii. Combined with precovery observations taken at the Samuel Oschin telescope in August 2003, and by the Near-Earth Asteroid Tracking consortium in 2001–2002, these observations allowed the accurate determination of its orbit. The calculations showed that the object was moving along a distant and highly eccentric orbit, at a distance of 90.3 AU from the Sun.<ref name="2004-E45"/><ref name="Mike"/> Precovery images have since been found in the Palomar Digitized Sky Survey dating back to 25 September 1990.<ref name="jpldata" />

NamingEdit

Brown initially nicknamed Sedna "The Flying Dutchman", or "Dutch", after a legendary ghost ship, because its slow movement had initially masked its presence from his team.<ref name="plutokiller">Template:Cite book</ref> He eventually settled on the official name after the goddess Sedna from Inuit mythology, partly because he mistakenly thought the Inuit were the closest polar culture to his home in Pasadena, and partly because the name, unlike Quaoar, would be easily pronounceable by English speakers.<ref name="plutokiller"/> Brown further justified his choice of naming by stating that the goddess Sedna's traditional location at the bottom of the Arctic Ocean reflected Sedna's large distance from the Sun.<ref name="mikebrown"/> He suggested to the International Astronomical Union's (IAU) Minor Planet Center that any objects discovered in Sedna's orbital region in the future should be named after mythical entities in Arctic mythologies.<ref name="mikebrown" />

The team made the name "Sedna" public before the object had been officially numbered, which caused some controversy among the community of amateur astronomers.<ref name="mpc">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> Brian Marsden, the head of the Minor Planet Center, stated that such an action was a violation of protocol, and that some members of the IAU might vote against it.<ref name="Walker"/> One amateur astronomer, Reiner Stoss, unsuccessfully attempted to name one of his asteroid discoveries "Sedna" (after the singer Katy Sedna) in protest of Brown's premature naming.<ref name="mpc"/><ref name="nyt">Template:Cite news</ref><ref name="planetx">Template:Cite book</ref> Despite the complaints by amateur astronomers, no objection was raised to Brown's name by members of the IAU and no competing names were suggested for Brown's object.<ref name="mpc"/> The IAU's Committee on Small Body Nomenclature accepted the name in September 2004,<ref name="MPC_20040928"/> and considered that, in similar cases of extraordinary interest, it might in the future allow names to be announced before they were officially numbered.<ref name="mpc"/>

Sedna has no symbol in astronomical literature, as the usage of planetary symbols is discouraged in astronomy. Unicode includes a symbol Template:Angbr (U+2BF2),<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> but this is mostly used among astrologers.<ref name=faulks>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> The symbol is a monogram of Template:Langx Sanna, the modern pronunciation of Sedna's name.<ref name=faulks/>

Orbit and rotationEdit

Sedna has the longest orbital period of any known object in the Solar System of its size or larger with an orbital period of around 11,400 years.<ref name="barycenter"/>Template:Refn Its orbit is extremely eccentric, with an aphelion of approximately 937 AU<ref name="barycenter"/> and a perihelion of 76.19 AU. Near aphelion, Sedna is one of the coldest places in the Solar System, located far past the termination shock, where temperatures never exceed −240°C (−400°F) due to its extreme distance.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> At aphelion, the Sun as viewed from Sedna is a particularly bright star, among the other stars, in the otherwise black sky, being about 45% as bright as the full moon as seen from Earth.<ref>Apparent magnitude of Sun at 937 AU = -26.74 + 5log(937) = -11.88

Full moon magnitude = -12.74

Ratio = 10^(0.4*(11.88-12.74)) = 0.453 ≈ 45%.</ref> Its perihelion was the largest for any known Solar System object until the discovery of the sednoid Template:Mpl.<ref name="Trujillo2007"/><ref name="Trujillo2014"/> At its aphelion, Sedna orbits the Sun at a meagre 377 m/s,<ref>Calculated: https://www.wolframalpha.com/input?i=G*solar+mass%2FAU%281%2F76.19-1%2F937%29%3D1%2F2*%28x+m%2Fs%29%5E2%28%28937%2F76.19%29%5E2-1%29</ref> 1.3% that of Earth's average orbital speed.<ref>377.4 m/s for Sedna divided by 29.78 km/s for Earth.</ref>

When Sedna was first discovered, it was 89.6 AU<ref name="AstDys2003"/> away from the Sun, approaching perihelion, and was the most distant object in the Solar System observed. Sedna was later surpassed by Eris, which was detected by the same survey near its aphelion at 97 AU. Because Sedna is near perihelion Template:As of, both Eris and Template:Dp are farther from the Sun, at 96 AU and 89 AU respectively, than Sedna at 84 AU, despite both of their semi-major axes being shorter than Sedna's.<ref name="AstDys-Eris" /><ref name="AstDys-OR10" /><ref name="AstDys" /> The orbits of some long-period comets extend further than that of Sedna; they are too dim to be discovered except when approaching perihelion in the inner Solar System. As Sedna nears its perihelion in mid-2076,<ref name="Perihelion2076"/>Template:Refn the Sun will appear merely as a very bright pinpoint in its sky, too far away to be visible as a disc to the naked eye.<ref name="HubbleSite2004image"/>

When first discovered, Sedna was thought to have an unusually long rotational period (20 to 50 days).<ref name="HubbleSite2004"/> It was initially speculated that Sedna's rotation was slowed by the gravitational pull of a large binary companion, similar to Pluto's moon Charon.<ref name="mikebrown" /> However, a search for such a satellite by the Hubble Space Telescope in March 2004 found no such objects.<ref name="HubbleSite2004"/>Template:Refn Subsequent measurements from the MMT telescope showed that Sedna in reality has a much shorter rotation period of about 10 hours, more typical for a body its size. It could rotate in about 18 hours instead, but this is thought to be unlikely.<ref name="Gaudi2005"/>

Physical characteristicsEdit

Sedna has a V band absolute magnitude of about 1.8, and is estimated to have an albedo (reflectivity) of around 0.41, giving it a diameter of approximately 900 km.<ref name=herschel/> At the time of discovery it was the brightest object found in the Solar System since Pluto in 1930. In 2004, the discoverers placed an upper limit of 1,800 km on its diameter;<ref name="Grundy2005"/> after observations by the Spitzer Space Telescope, this was revised downward by 2007 to less than 1,600 km.<ref name="spitzer"/> In 2012, measurements from the Herschel Space Observatory suggested that Sedna's diameter was Template:Nowrap, which would make it smaller than Pluto's moon Charon.<ref name=herschel>Template:Cite journal</ref> In 2013, the same team re-analyzed Sedna's thermal data with an improved thermophysical model and found a consistent value of Template:Val, suggesting that the original model fit was too precise.<ref name="Lellouch A60">Template:Cite journal</ref> Australian observations of a stellar occultation by Sedna in 2013 produced similar results on its diameter, giving chord lengths Template:Val and Template:Val.<ref name="Rommel2020"/> The size of this object suggests it could have undergone differentiation and may have a sub-surface liquid ocean and possibly geologic activity.<ref name="Emery2007"/>

As Sedna has no known moons, the direct determination of its mass is as yet impossible without either sending a space probe or perhaps locating a nearby object which is gravitationally perturbed by the planetoid. It is the largest trans-Neptunian Sun-orbiting object not known to have a natural satellite.<ref name = "Lakdawalla2016a" /> As of 2024, observations from the Hubble Space Telescope in 2004 have been the only published attempt to find a satellite,<ref name="HubbleProposal" /><ref name="Mystery" /> and it is possible that a satellite could have been lost in the glare from Sedna itself.<ref name="BannisterTwitter" />

Observations from the SMARTS telescope show that Sedna, in visible light, is one of the reddest objects known in the Solar System, nearly as red as Mars.<ref name="mikebrown"/> Its deep red spectral slope is indicative of high concentrations of organic material on its surface.<ref name="Emery2007" /> Chad Trujillo and his colleagues suggest that Sedna's dark red color is caused by an extensive surface coating of hydrocarbon sludge, termed tholins. Tholins are a reddish-colored, amorphous, and heterogeneous organic mixture hypothesized to have been transmuted from simpler organic compounds, following billions of years of continuous exposure to ultraviolet radiation, interstellar particles, and other harsh environs as the dwarf planet either comes close to the Sun or transits interstellar space.<ref name="Trujillo2005"/> Its surface is homogeneous in color and spectrum; this may be because Sedna, unlike objects nearer the Sun, is rarely impacted by other bodies, which would expose bright patches of fresh icy material like that on 8405 Asbolus.<ref name="Trujillo2005"/> Sedna and two other very distant objects – Template:Mpl and Template:Mpl – share their color with outer classical Kuiper belt objects and the centaur 5145 Pholus, suggesting a similar region of origin.<ref name="Sheppard2010"/>

Trujillo and colleagues have placed upper limits on Sedna's surface composition of 60% for methane ice and 70% for water ice.<ref name="Trujillo2005"/> The presence of methane further supports the existence of tholins on Sedna's surface, as methane is among the organic compounds capable of giving rise to tholins.<ref name="Emery2007"/> Barucci and colleagues compared Sedna's spectrum with that of Triton and detected weak absorption bands belonging to methane and nitrogen ices. From these observations, they suggested the following model of the surface: 24% Triton-type tholins, 7% amorphous carbon, 10% nitrogen ices, 26% methanol, and 33% methane.<ref name="Triton"/> The detection of methane and water ice was confirmed in 2006 by the Spitzer Space Telescope mid-infrared photometry.<ref name="Emery2007"/> The European Southern Observatory's Very Large Telescope observed Sedna with the SINFONI near-infrared spectrometer, finding indications of tholins and water ice on the surface.<ref name="Barucci_et_al_2010">Template:Cite journal</ref>

In 2022, low-resolution near-infrared (0.7–5 μm) spectroscopic observations by the James Webb Space Telescope (JWST) revealed the presence of significant amounts of ethane ice (C₂H₆) and of complex organics on the surface of Sedna. The JWST spectra also contain evidence of the existence of small amounts of ethylene (C₂H₄), acetylene (C₂H₂) and possibly carbon dioxide (CO₂). On the other hand little evidence of the existence of methane (CH₄) and nitrogen ices was found at variance with the earlier observations.<ref name="Emery2024"/>

The possible presence of nitrogen on the surface suggests that, at least for a short time, Sedna may have a tenuous atmosphere. During the 200-year portion of its orbit near perihelion, the maximum temperature on Sedna should exceed Template:Convert, the transition temperature between alpha-phase solid N₂ and the beta-phase seen on Triton. At 38 K, the N₂ vapor pressure would be 14 microbar (1.4 Pa). The weak methane absorption bands indicate that methane on Sedna's surface is ancient, as opposed to being freshly deposited. This finding indicates that Sedna's surface never reaches a temperature high enough for methane on the surface to evaporate and subsequently fall back as snow, which happens on Triton and probably on Pluto.<ref name="Emery2007"/>

OriginEdit

In their paper announcing the discovery of Sedna, Brown and his colleagues described it as the first observed body belonging to the Oort cloud, the hypothetical cloud of comet-like objects thought to exist out to nearly a light-year from the Sun. They observed that, unlike scattered disc objects such as Eris, Sedna's perihelion (76 AU) is too distant for it to have been scattered by the gravitational influence of Neptune.<ref name="Mike"/> Because it is considerably closer to the Sun than was expected for an Oort cloud object, and has an inclination roughly in line with the planets and the Kuiper belt, they described the planetoid as being an "inner Oort cloud object", situated in the disc reaching from the Kuiper belt to the spherical part of the cloud.<ref name="Swiss" /><ref name="LykDyn"/>

If Sedna formed in its current location, the Sun's original protoplanetary disc must have extended as far as 75 AU into space.<ref name="SternAJ2005"/> On top of that, Sedna's initial orbit must have been approximately circular, otherwise its formation by the accretion of smaller bodies into a whole would not have been possible, because the large relative velocities between planetesimals would have been too disruptive. Therefore, it must have been tugged into its current eccentric orbit by a gravitational interaction with another body.<ref name="scattered"/> In their initial paper, Brown, Rabinowitz and colleagues suggested three possible candidates for the perturbing body: an unseen planet beyond the Kuiper belt, a single passing star, or one of the young stars embedded with the Sun in the stellar cluster in which it formed.<ref name="Mike"/>

Brown and his team favored the hypothesis that Sedna was lifted into its current orbit by a star from the Sun's birth cluster, arguing that Sedna's aphelion of about 1,000 AU, which is relatively close compared to those of long-period comets, is not distant enough to be affected by passing stars at their current distances from the Sun. They propose that Sedna's orbit is best explained by the Sun having formed in an open cluster of several stars that gradually disassociated over time.<ref name="Mike"/><ref name="Brown2004AAS205"/><ref name="PlanetarySociety"/> That hypothesis has also been advanced by both Alessandro Morbidelli and Scott Jay Kenyon.<ref name="Morbidelli2004"/><ref name="Kenyon2004"/> Computer simulations by Julio A. Fernandez and Adrian Brunini suggest that multiple close passes by young stars in such a cluster would pull many objects into Sedna-like orbits.<ref name="Mike"/> A study by Morbidelli and Levison suggested that the most likely explanation for Sedna's orbit was that it had been perturbed by a close (approximately 800 AU) pass by another star in the first 100 million years or so of the Solar System's existence.<ref name="Morbidelli2004"/><ref name="challenge"/>

File:Trans-Neptunians Size Albedo Color.svg

Comparison of sizes, albedo, and colors of various large trans-Neptunian objects with sizes of >700 km. The dark colored arcs represent uncertainties of the object's size.

The trans-Neptunian planet hypothesis has been advanced in several forms by numerous astronomers, including Rodney Gomes and Patryk Lykawka. One scenario involves perturbations of Sedna's orbit by a hypothetical planetary-sized body in the inner Oort cloud. In 2006, simulations suggested that Sedna's orbital traits could be explained by perturbations of a Jupiter-mass (Template:Jupiter mass) object at 5,000 AU (or less), a Neptune-mass object at 2,000 AU, or even an Earth-mass object at 1,000 AU.<ref name="PlanetarySociety"/><ref name="Gomez2006"/> Computer simulations by Patryk Lykawka have indicated that Sedna's orbit may have been caused by a body roughly the size of Earth, ejected outward by Neptune early in the Solar System's formation and currently in an elongated orbit between 80 and 170 AU from the Sun.<ref name="lykawka"/> Brown's various sky surveys have not detected any Earth-sized objects out to a distance of about 100 AU. It's a possibility that such an object may have been scattered out of the Solar System after the formation of the inner Oort cloud.<ref name="sisters"/>

Caltech researchers Konstantin Batygin and Mike Brown have hypothesized the existence of a super-Earth planet in the outer Solar System—Planet Nine—to explain the orbits of a group of extreme trans-Neptunian objects that includes Sedna.<ref name="Evidence for a Distant Giant Planet"/><ref>Template:Cite press release</ref> This planet would be perhaps six times as massive as Earth.<ref name="Brown_Batygin_2021z">Template:Cite journal</ref> It would have a highly eccentric orbit, and its average distance from the Sun would be about 15 times that of Neptune (which orbits at an average distance of Template:Convert). Accordingly, its orbital period would be approximately 7,000 to 15,000 years.<ref name="Brown_Batygin_2021z"/>

Morbidelli and Kenyon have suggested that Sedna did not originate in the Solar System, but was captured by the Sun from a passing extrasolar planetary system, specifically that of a brown dwarf about 1/20th the mass of the Sun (Template:Solar mass)<ref name="Morbidelli2004" /><ref name="Kenyon2004" /><ref>Template:Cite journal</ref> or a main-sequence star 80 percent more massive than the Sun, which, owing to its larger mass, may now be a white dwarf. In either case, the stellar encounter had likely occurred within 100 million years after the Sun's formation.<ref name="Morbidelli2004" /><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> Stellar encounters during this time would have minimal effect on the Oort cloud's final mass and population since the Sun had excess material for replenishing the Oort cloud.<ref name="Morbidelli2004" />

PopulationEdit

{{#invoke:Labelled list hatnote|labelledList|Main article|Main articles|Main page|Main pages}}

File:Sednoid orbits.png

Orbit diagram of Sedna, Template:Mpl, and Leleākūhonua with 100 AU grids for scale

Sedna's highly elliptical orbit, and thus a narrow temporal window for detection and observation with currently available technology, means that the probability of its detection was roughly 1 in 80. Unless its discovery were a fluke, it is expected that another 40–120 Sedna-sized objects with roughly the same orbital parameters would exist in the outer solar system.<ref name="Mike" /><ref name="largest" />

In 2007, astronomer Megan Schwamb outlined how each of the proposed mechanisms for Sedna's extreme orbit would affect the structure and dynamics of any wider population. If a trans-Neptunian planet was responsible, all such objects would share roughly the same perihelion (about 80 AU). If Sedna was captured from another planetary system that rotated in the same direction as the Solar System, then all of its population would have orbits on relatively low inclinations and have semi-major axes ranging from 100 to 500 AU. If it rotated in the opposite direction, then two populations would form, one with low and one with high inclinations. The perturbations from passing stars would produce a wide variety of perihelia and inclinations, each dependent on the number and angle of such encounters.<ref name="sisters"/>

A larger sample of objects with Sedna's extreme perihelion may help in determining which scenario is most likely.<ref name="Schwamb"/> "I call Sedna a fossil record of the earliest Solar System", said Brown in 2006. "Eventually, when other fossil records are found, Sedna will help tell us how the Sun formed and the number of stars that were close to the Sun when it formed."<ref name="fussman"/> A 2007–2008 survey by Brown, Rabinowitz, and Megan Schwamb attempted to locate another member of Sedna's hypothetical population. Although the survey was sensitive to movement out to 1,000 AU and discovered the likely dwarf planet Gonggong, it detected no new sednoid.<ref name="Schwamb" /> Subsequent simulations incorporating the new data suggested about 40 Sedna-sized objects probably exist in this region, with the brightest being about Eris's magnitude (−1.0).<ref name="Schwamb"/>

In 2014, Chad Trujillo and Scott Sheppard announced the discovery of Template:Mpl,<ref name="Trujillo2014"/> an object half the size of Sedna, a 4,200-year orbit similar to Sedna's, and a perihelion within Sedna's range of roughly 80 AU;<ref name="jpldata 2012 VP113"/> they speculated that this similarity of orbits may be due to the gravitational shepherding effect of a trans-Neptunian planet.<ref name="Physorg"/> Another high-perihelion trans-Neptunian object was announced by Sheppard and colleagues in 2018, provisionally designated Template:Mp and now named Leleākūhonua.<ref name="Carnegie2018"/> With a perihelion of 65 AU and an even more distant orbit with a period of 40,000 years, its longitude of perihelion (the location where it makes its closest approach to the Sun) appears to be aligned with the directions of both Sedna and Template:Mp, strengthening the case for an apparent orbital clustering of trans-Neptunian objects suspected to be influenced by a hypothetical distant planet, dubbed Planet Nine. In a study detailing Sedna's population and Leleākūhonua's orbital dynamics, Sheppard concluded that the discovery implies a population of about 2 million inner Oort Cloud objects larger than 40 km, with a total mass in the range of Template:Val (several times the mass of the asteroid belt and 80% the mass of Pluto).<ref name="Sheppard-2019"/>

Sedna was recovered from Transiting Exoplanet Survey Satellite data in 2020, as part of preliminary work for an all-sky survey searching for Planet Nine and other as-yet-unknown trans-Neptunian objects.<ref name="Rice_Laughlin_TESS_2020">Template:Cite journal</ref>

ClassificationEdit

The discovery of Sedna renewed the old question of just which astronomical objects ought to be considered planets, and which ones ought not to be. On 15 March 2004, articles on Sedna in the popular press reported misleadingly that a tenth planet had been discovered. This question was resolved for many astronomers by applying the International Astronomical Union's definition of a planet, adopted on 24 August 2006, which mandated that a planet must have cleared the neighborhood around its orbit. Sedna is not expected to have cleared its neighborhood; quantitatively speaking, its Stern–Levison parameter is estimated to be much less than 1.Template:Refn The IAU also adopted dwarf planet as a term for the largest non-planets (despite the name) that, like planets, are in hydrostatic equilibrium and thus can display planet-like geological activity, yet have not cleared their orbital neighborhoods.<ref name=planetarysociety>Template:Cite journal</ref> Sedna is bright enough, and therefore large enough, that it is expected to be in hydrostatic equilibrium.<ref>Template:Cite journal</ref> Hence, astronomers generally consider Sedna a dwarf planet.<ref name="Barucci_et_al_2010"/><ref>Template:Cite journal</ref><ref>Template:Cite journal</ref><ref name="Tancredi2008"/><ref name="Brown-dplist" /><ref name="Grundy2019">Template:Cite journal</ref> The list of dwarf planets recognized by the IAU has not changed since 2006, even though Sedna is considered to be one by most astronomers.<ref>Template:Citation</ref>

Besides its physical classification, Sedna is also categorized according to its orbit. The Minor Planet Center, which officially catalogs the objects in the Solar System, designates Sedna only as a trans-Neptunian object (as it orbits beyond Neptune),<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> as does the JPL Small-Body Database.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> The question of a more precise orbital classification has been much debated, and many astronomers have suggested that the sednoids, together with similar objects such as Template:Mpl, be placed in a new category of distant objects named extended scattered disc objects (E-SDO),<ref name="Gladman" /> detached objects,<ref name="Jewitt2006"/> distant detached objects (DDO),<ref name="Gomez2006" /> or scattered-extended in the formal classification by the Deep Ecliptic Survey.<ref name="DES_Elliot2006"/>

ExplorationEdit

Sedna will come to perihelion around July 2076.<ref name="Perihelion2076"/><ref group=lower-alpha name=footnoteC/> This close approach to the Sun provides a window of opportunity for studying it that will not occur again for more than 11 millennia. Because Sedna spends much of its orbit beyond the heliopause, the point at which the solar wind gives way to the interstellar particle wind, examining Sedna's surface would provide unique information on the effects of interstellar radiation, as well as the properties of the solar wind at its farthest extent.<ref>Template:Cite journal</ref> It was calculated in 2011 that a flyby mission to Sedna could take 24.48 years using a Jupiter gravity assist, based on launch dates of 6 May 2033 or 23 June 2046. Sedna would be either 77.27 or 76.43 AU from the Sun when the spacecraft arrives near the end of 2057 or 2070, respectively.<ref name=McGranaghan/> Other potential flight trajectories involve gravity assists from Venus, Earth, Saturn, and Neptune as well as Jupiter.<ref>Template:Cite journal</ref> Research at the University of Tennessee has also examined the potential for a lander.<ref>Template:Cite journal</ref>