Sedna as imaged by the Hubble Space Telescope
|Discovered by||Michael E. Brown,
|Discovery date||November 14, 2003|
|MPC designation||90377 Sedna|
|Alternative names||2003 VB12|
|Minor planet category||trans-Neptunian object
Oort cloud object
|Epoch 2010-Jul-23 (JD 2455400.5)|
|Aphelion||937 AU (Q)
|Perihelion||76.361 AU (q)
1.142 3×1013 m
|Semi-major axis||518.57 AU (a)
7.757 6×1013 m
|Orbital period||≈11,400 yr[a]|
|Average orbital speed||1.04 km/s|
|Longitude of ascending node||144.26°|
|Argument of perihelion||311.02°|
|Dimensions||995 ± 80 km|
|Mass||≈1 × 1021 kg[b]|
|Equatorial surface gravity||≈0.27 m/s2|
|Escape velocity||≈0.518 km/s|
|Sidereal rotation period||0.42 d (10 h)|
|Albedo||0.32 ± 0.06 |
|Temperature||≈12 K (see note here)|
|Spectral type||(red) B−V=1.24; V−R=0.78|
|Absolute magnitude (H)||1.83 ± 0.05 |
90377 Sedna is a large trans-Neptunian object, which as of 2012[update] was about three times as far from the Sun as Neptune. Spectroscopy has revealed that Sedna's surface composition is similar to that of some other trans-Neptunian objects, being largely a mixture of water, methane and nitrogen ices with tholins. Its surface is one of the reddest in the Solar System. It is believed to be a dwarf planet by several astronomers, and is large enough to be considered one under the 2006 draft proposal of the IAU, though the IAU has not formally recognized it as such.
For most of its orbit it is even farther from the Sun than at present, with its aphelion estimated at 937 astronomical units (31 times Neptune's distance), making it one of the most distant known objects in the Solar System other than long-period comets.[c][d] Sedna's exceptionally long and elongated orbit, taking approximately 11,400 years to complete, and distant point of closest approach to the Sun, at 76 AU, have led to much speculation as to its origin. The Minor Planet Center currently places Sedna in the scattered disc, a group of objects sent into highly elongated orbits by the gravitational influence of Neptune. However, this classification has been contested, as Sedna never comes close enough to Neptune to have been scattered by it, leading some astronomers to conclude that it is in fact the first known member of the inner Oort cloud. Others speculate that it might have been tugged into its current orbit by a passing star, perhaps one within the Sun's birth cluster, or even that it was captured from another star system. Another hypothesis suggests that its orbit may be evidence for a large planet beyond the orbit of Neptune. Astronomer Michael E. Brown, co-discoverer of Sedna and the dwarf planets Eris, Haumea, and Makemake, believes it to be the most scientifically important trans-Neptunian object found to date, as understanding its unusual orbit is likely to yield valuable information about the origin and early evolution of the Solar System.
Discovery and naming
Sedna (provisionally designated 2003 VB12) was discovered by Mike Brown (Caltech), Chad Trujillo (Gemini Observatory) and David Rabinowitz (Yale University) on November 14, 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 in November–December 2003 with the SMARTS telescope at Cerro Tololo Inter-American Observatory in Chile as well as with the Tenagra IV telescope at the W. M. Keck Observatory in Hawaii revealed that the object was moving along a distant highly eccentric orbit. Later the object was identified on older precovery images made by the Samuel Oschin telescope as well as on images from the Near Earth Asteroid Tracking consortium. These previous positions expanded its known orbital arc and allowed a more precise calculation of its orbit.
"Our newly discovered object is the coldest most distant place known in the Solar System," said Mike Brown on his website, "so we feel it is appropriate to name it in honor of Sedna, the Inuit goddess of the sea, who is thought to live at the bottom of the frigid Arctic Ocean." Brown also suggested to the International Astronomical Union's (IAU) Minor Planet Center that any future objects discovered in Sedna's orbital region should also be named after entities in arctic mythologies. The team made the name "Sedna" public before the object had been officially numbered. Brian Marsden, the head of the Minor Planet Center, said that such an action was a violation of protocol, and that some members of the IAU might vote against it. However, no objection was raised to the name, and no competing names were suggested. The IAU's Committee on Small Body Nomenclature formally accepted the name in September 2004, and also considered that, in similar cases of extraordinary interest, it might in the future allow names to be announced before they were officially numbered.
Orbit and rotation
Sedna has the longest orbital period of any known large object in the Solar System[d], calculated at around 11,400 years.[a] Its orbit is extremely eccentric, with an aphelion estimated at 937 AU and a perihelion at about 76 AU, the most distant perihelion ever observed for any Solar System object. At its discovery it was 89.6 AU from the Sun approaching perihelion, and was the most distant object in the Solar System yet observed. Eris was later detected by the same survey at 97 AU. Although the orbits of some long-period comets extend farther than that of Sedna, they are too dim to be discovered except when approaching perihelion in the inner Solar System. Even as Sedna nears its perihelion in mid 2076,[e] the Sun would appear merely as a very bright star in its sky, only 100 times brighter than a full Moon on Earth, and too far away to be visible as a disc to the naked eye.
When first discovered, Sedna was thought to have an unusually long rotational period (20 to 50 days). 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. A search for such a satellite by the Hubble Space Telescope in March 2004 found nothing,[f] and subsequent measurements from the MMT telescope suggest a much shorter rotation period of about 10 hours; rather typical for a body of its size.
Sedna has a V-band absolute magnitude (H) of about 1.8, and it is estimated to have an albedo of about 0.32, thus giving it a diameter of approximately 1,000 km. At the time of its discovery it was the intrinsically 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, but by 2007 this was revised downward to less than 1,600 km after observation by the Spitzer Space Telescope. In 2012, measurements from the Herschel Space Observatory suggested that Sedna's diameter was 995 ± 80 km, which would make it smaller than Pluto's moon Charon. As Sedna has no known moons, determining its mass is currently impossible without sending a space probe. However, if the above estimates for its diameter are coupled with Pluto's density of 2.0 g/cm3, the resultant estimated mass range is about 1 × 1021 kg.[b]
Observations from the SMARTS telescope show that in visible light Sedna is one of the reddest objects in the Solar System, nearly as red as Mars. Chad Trujillo and his colleagues suggest that Sedna's dark red colour is caused by a surface coating of hydrocarbon sludge, or tholin, formed from simpler organic compounds after long exposure to ultraviolet radiation. Its surface is homogeneous in colour 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. Sedna and two other very distant objects ((87269) 2000 OO67 and 2006 SQ372) share their colour with outer classical Kuiper belt objects and the centaur 5145 Pholus, suggesting a similar region of origin.
Trujillo and colleagues have placed upper limits in Sedna's surface composition of 60% for methane ice and 70% for water ice. The presence of methane further supports the existence of tholins on Sedna's surface, as they are produced by irradiation of methane. 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, 26% methanol and 33% methane. The detection of methane and water ices was confirmed in 2006 by Spitzer Space Telescope mid-infrared photometry. The presence of nitrogen on the surface suggests the possibility that, at least for a short time, Sedna may possess an atmosphere. During a 200-year period near perihelion the maximum temperature on Sedna should exceed 35.6 K (−237.6 °C), 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 (0.000014 Atmospheres). However, its deep red spectral slope is indicative of high concentrations of organic material on its surface, and its weak methane absorption bands indicate that methane on Sedna's surface is ancient, rather than freshly deposited. This means that Sedna is too cold for methane to evaporate from its surface and then fall back as snow, as happens on Triton and probably on Pluto.
In their paper announcing the discovery of Sedna, Mike Brown and his colleagues described it as the first observed body belonging to the Oort cloud, the hypothetical cloud of comets thought to exist 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. Because it is a great deal 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.
If Sedna formed in its current location, the Sun's original protoplanetary disc must have extended as far as 75 AU into space. Also, Sedna's initial orbit must have been circular, otherwise its formation by the accretion of smaller bodies into a whole would not have been possible, as 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. 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.
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. That hypothesis has also been advanced by both Alessandro Morbidelli and Scott Jay Kenyon. 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. A study by Morbidelli and Hal 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.
The trans-Neptunian planet hypothesis has been advanced in several forms by a number of 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. Recent simulations show that Sedna's orbital traits could be explained by perturbations by a Neptune-mass object at 2,000 AU (or less), a Jupiter-mass at 5,000 AU, or even an Earth-mass object at 1,000 AU. Computer simulations by Patryk Lykawka have suggested 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. Mike Brown's various sky surveys have not detected any Earth-sized objects out to a distance of about 100 AU. However, it is possible that such an object may have been scattered out of the Solar System after the formation of the inner Oort cloud.
It has been suggested that Sedna's orbit is the result of influence by a large binary companion to the Sun, thousands of AU distant. One such hypothetical companion is Nemesis, a dim companion to the Sun which has been proposed to be responsible for the supposed periodicity of mass extinctions on Earth from cometary impacts, the lunar impact record, and the common orbital elements of a number of long-period comets. However, to date no direct evidence of Nemesis has been found, and many lines of evidence (such as crater counts), have thrown its existence into doubt. John J. Matese and Daniel P. Whitmire, longtime proponents of the possibility of a wide binary companion to the Sun, have suggested that an object of five times the mass of Jupiter lying at roughly 7850 AU from the Sun could produce a body in Sedna's orbit.
Morbidelli and Scott Jay Kenyon have also suggested that Sedna did not originate in our 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.
Sedna's highly elliptical orbit means that the probability of its detection was roughly 1 in 80, suggesting that, unless its discovery was a fluke, another 40–120 Sedna-sized objects would exist within its region. Another object, 2000 CR105, has a similar but less extreme orbit: it has a perihelion of 44.3 AU, an aphelion of 394 AU, and an orbital period of 3,240 years. It may have been affected by the same processes as Sedna.
Each of the proposed mechanisms for Sedna's extreme orbit would leave a distinct mark on the structure and dynamics of any wider population. If a trans-Neptunian planet was responsible, all such objects would share roughly the same perihelion (≈80 AU). If Sedna were captured from another planetary system that rotated in the same direction as the Solar System, then Sedna's population would all possess relatively low inclinations and possess semi-major axes ranging from 100–500 AU. If it rotated in the opposite direction, then two populations would form, one with low inclinations and one with high. The gravity of perturbing stars would produce a wide variety of perihelia and inclinations, each dependent on the number and angle of such encounters.
Gaining a larger sample of such objects could therefore help in determining which scenario is most likely. "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." 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 2007 OR10, it detected no new bodies in Sedna-like orbits. Subsequent simulations incorporating the new data suggested about 40 Sedna-sized objects probably exist in this region.
The Minor Planet Center, which officially catalogs the objects in the Solar System, classifies Sedna as a scattered object. However, this grouping is heavily questioned, and many astronomers have suggested that it, together with a few other objects (e.g. 2000 CR105), be placed in a new category of distant objects named extended scattered disc objects (E-SDO), detached objects, distant detached objects (DDO) or scattered-extended in the formal classification by the Deep Ecliptic Survey.
The discovery of Sedna resurrected the question of which astronomical objects should be considered planets and which should not. On March 15, 2004, articles on Sedna in the popular press reported that a tenth planet had been discovered. This question was answered under the International Astronomical Union definition of a planet, adopted on August 24, 2006, which mandated that a planet must have cleared the neighborhood around its orbit. Sedna has a Stern–Levison parameter estimated to be much less than 1,[g] and therefore cannot be considered to have cleared the neighborhood, even though no other objects have yet been discovered in its vicinity. To qualify as a dwarf planet, Sedna must be shown to be in hydrostatic equilibrium. It is bright enough, and therefore large enough, that this is expected to be the case.
Sedna's perihelion will be reached around 2075–2076.[e] This close approach to the Sun provides an opportunity of study which will not occur again for 12,000 years. Though Sedna is listed on NASA's Solar System exploration website, NASA is not known to be considering any type of mission at this time.
- Given the orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the orbital period. Using a 1950 epoch, Sedna shows a 12,100-year period, but using a 2010 epoch Sedna shows a 11,800-year period. For objects at such high eccentricity, the Sun's barycentric coordinates are more stable than heliocentric coordinates. Using JPL Horizons, the barycentric orbital period is approximately 11,400 years.
- Taking Herschel's estimates for the diameter of about 1,000 km and assuming Pluto's density of 2.0 (<0.10 Eris)
- As of 2012[update], Sedna was about 87 AU from the Sun; Eris, the most massive known dwarf planet, is currently farther from the Sun than Sedna at 96.6 AU. Eris is near its aphelion (furthest distance from the Sun), while Sedna is nearing its 2076 perihelion (closest approach to the Sun). Sedna will overtake Eris in 2114, but the probable dwarf planet 2007 OR10 will overtake both of them by 2045.
- Small Solar System bodies such as 2010 EC46, (308933) 2006 SQ372, 2005 VX3, (87269) 2000 OO67, 2002 RN109, 2007 TG422, and several comets (such as the Great Comet of 1577) have larger heliocentric orbits. But only (308933) 2006 SQ372, (87269) 2000 OO67, and 2007 TG422 have a perihelion point further than Jupiter's orbit, so it is debatable whether or not most of these objects are misclassified comets.
- Different programs using different epochs and/or data sets will produce slightly different dates for Sedna's perihelion. Using a 2010 epoch, the JPL small body database shows a perihelion date of 2075. Using a 1990 epoch the Lowell DES shows perihelion on 2479285.0598 (2075-12-13) As of 2010[update], the JPL Horizons (using numerical integration) showed a perihelion date of 2076-Jul-18.
- The HST search found no satellite candidates to a limit of about 500 times fainter than Sedna (Brown and Suer 2007).
- The Stern–Levison parameter (Λ) as defined by Alan Stern and Harold F. Levison in 2002 determines if an object will eventually clear its orbital neighbourhood of small bodies. It is defined as the object's fraction of solar mass (i.e., the object's mass divided by the Sun's mass) squared, divided by its semi-major axis to the 3/2 power, times a constant 1.7×1016.(see equation 4) If an object's Λ is greater than 1, then that object will eventually clear its neighbourhood, and it can be considered for planethood. Using the unlikely highest estimated mass for Sedna of 2×1021 kg, Sedna's Λ is (2×1021/1.9891×1030)2 / 5193/2 × 1.7×1016 = 1.44×10−6. This is much less than 1, so Sedna is not a planet by this criterion.
- "Discovery Circumstances: Numbered Minor Planets (90001)–(95000)". IAU: Minor Planet Center. Retrieved 2008-07-23.
- Marc W. Buie (2009-11-22). "Orbit Fit and Astrometric record for 90377". Deep Ecliptic Survey. Retrieved 2006-01-17.
- Horizons output. "Barycentric Osculating Orbital Elements for 90377 Sedna (2003 VB12)". Retrieved 2011-04-30. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0) (saved Horizons output file 2011-Feb-04)
- "JPL Small-Body Database Browser: 90377 Sedna (2003 VB12)". 2010-01-05 last obs. Retrieved 2008-06-11.
- Kaib, Nathan A.; Becker, Andrew C.; Jones, R. Lynne; Puckett, Andrew W.; Bizyaev, Dmitry; Dilday, Benjamin; Frieman, Joshua A.; Oravetz, Daniel J.; Pan, Kaike; Quinn, Thomas; Schneider, Donald P.; Watters, Shannon (2009). "2006 SQ372: A Likely Long-Period Comet from the Inner Oort Cloud". The Astrophysical Journal 695 (1): 268–275. arXiv:0901.1690. Bibcode:2009ApJ...695..268K. doi:10.1088/0004-637X/695/1/268.
- Pál, A.; Kiss, C.; Müller, T. G.; Santos-Sanz, P.; Vilenius, E.; Szalai, N.; Mommert, M.; Lellouch, E. et al. (2012). ""TNOs are Cool": A survey of the trans-Neptunian region. VII. Size and surface characteristics of (90377) Sedna and 2010 EK139". Astronomy & Astrophysics 541: L6. arXiv:1204.0899. Bibcode:2012A&A...541L...6P. doi:10.1051/0004-6361/201218874.
- "Case of Sedna's Missing Moon Solved". Harvard-Smithsonian Center for Astrophysics. 2005-04-05. Retrieved 2005-04-07.
- Stephen C. Tegler (2006-01-26). "Kuiper Belt Object Magnitudes and Surface Colors". Northern Arizona University. Retrieved 2006-11-05.
- "AstDys (90377) Sedna Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2011-05-05.
- JPL Horizons On-Line Ephemeris System (2010-07-18). "Horizons Output for Sedna 2076/2114". Retrieved 2010-07-18. Horizons
- Barucci, et al. (2010). "(90377) Sedna: Investigation of surface compositional variation". The Astronomical Journal 140: 6.
- Rabinowitz, Schaefer, Tourtellotte, 2011. "SMARTS Studies of the Composition and Structure of Dwarf Planets". Bulletin of the American Astronomical Society, Vol. 43
- Malhotra, 2010. "On the Importance of a Few Dwarf Planets". Bulletin of the American Astronomical Society, Vol. 41
- Tancredi, G.; Favre, S. (2008). "Which are the dwarfs in the solar system?". Asteroids, Comets, Meteors. Retrieved 2011-01-05.
- Michael E. Brown (Sep 23 2011). "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 2011-09-23.
- O. Gingerich (2006). "The Path to Defining Planets" (PDF). Harvard-Smithsonian Center for Astrophysics and IAU EC Planet Definition Committee chair. Retrieved 2007-03-13.
- "Planetary Names: Planet and Satellite Names and Discoverers". Gazetteer of Planetary Nomenclature. International Astronomical Union (Working Group for Planetary System Nomenclature). Retrieved 10 June 2012.
- NASA. "List of Dwarf Planets". Retrieved 2012-06-09.
- "AstDys (136199) Eris Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 4 June 2011. Retrieved 2011-05-05.
- Cal Fussman (2006). "The Man Who Finds Planets". Discover. Archived from the original on 16 June 2010. Retrieved 2010-05-22.
- Mike Brown, David Rabinowitz, Chad Trujillo (2004). "Discovery of a Candidate Inner Oort Cloud Planetoid". Astrophysical Journal 617 (1): 645–649. arXiv:astro-ph/0404456. Bibcode:2004ApJ...617..645B. doi:10.1086/422095.
- Brown, Mike. "Sedna". Caltech. Archived from the original on 25 July 2010. Retrieved 2010-07-20.
- "MPEC 2004-S73 : Editorial Notice". IAU Minor Planet Center. 2004. Retrieved 2010-07-18.
- Walker, Duncan (2004-03-16). "How do planets get their names?". BBC News. Retrieved 2010-05-22.
- "MPC 52733". Minor Planet Center. 2004. Retrieved 2010-08-30.
- Chadwick A. Trujillo, M. E. Brown, D. L. Rabinowitz; Brown; Rabinowitz (2007). "The Surface of Sedna in the Near-infrared". Bulletin of the American Astronomical Society 39: 510. Bibcode:2007DPS....39.4906T.
- "AstDys (90377) Sedna Ephemerides 2003-11-14". Department of Mathematics, University of Pisa, Italy. Retrieved 2008-05-05.
- "Hubble Observes Planetoid Sedna, Mystery Deepens; Long View from a Lonely Planet". Hubblesite, STScI-2004-14. 2004. Retrieved 2010-07-21.
- "Hubble Observes Planetoid Sedna, Mystery Deepens". Hubblesite, STScI-2004-14. 2004. Retrieved 2010-08-30.
- Michael E. Brown. "The largest Kuiper belt objects" (pdf). In M. Antonietta Barucci, Hermann Boehnhardt, Dale P. Cruikshank. The Solar System Beyond Neptune. University of Arizona Press. pp. 335–345. ISBN 0-8165-2755-5.
- B. Scott Gaudi; Krzysztof Z. Stanek, Joel D. Hartman, Matthew J. Holman, Brian A. McLeod (CfA) (2005). "On the Rotation Period of (90377) Sedna". The Astrophysical Journal 629 (1): L49–L52. arXiv:astro-ph/0503673. Bibcode:2005ApJ...629L..49G. doi:10.1086/444355.
- W. M. Grundy, K. S. Noll, D. C. Stephens (2005). "Diverse Albedos of Small Trans-Neptunian Objects". Icarus (Lowell Observatory, Space Telescope Science Institute) 176 (1): 184–191. arXiv:astro-ph/0502229. Bibcode:2005Icar..176..184G. doi:10.1016/j.icarus.2005.01.007.
- John Stansberry, Will Grundy, Mike Brown, Dale Cruikshank, John Spencer, David Trilling, Jean-Luc Margot (2008). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope" (pdf). In M. Antonietta Barucci, Hermann Boehnhardt, Dale P. Cruikshank. The Solar System Beyond Neptune. University of Arizona Press. pp. 161–179. arXiv:astro-ph/0702538v2. ISBN 0-8165-2755-5.
- Trujillo, Chadwick A.; Brown, Michael E.; Rabinowitz, David L.; Geballe, Thomas R. (2005). "Near‐Infrared Surface Properties of the Two Intrinsically Brightest Minor Planets: (90377) Sedna and (90482) Orcus". The Astrophysical Journal 627 (2): 1057–1065. arXiv:astro-ph/0504280. Bibcode:2005ApJ...627.1057T. doi:10.1086/430337.
- Sheppard, Scott S. (2010). "The colors of extreme outer Solar System objects". The Astronomical Journal 139 (4): 1394–1405. arXiv:1001.3674. Bibcode:2010AJ....139.1394S. doi:10.1088/0004-6256/139/4/1394.
- J. P. Emery, C. M. Dalle Ore, D. P. Cruikshank, Fernández, Y. R., Trilling, D. E., Stansberry, J. A. (2007). "Ices on 90377 Sedna: Conformation and compositional constraints" (pdf). Astronomy and Astrophysics 406 (1): 395–398. Bibcode:2007A&A...466..395E. doi:10.1051/0004-6361:20067021.
- M. A. Barucci, D. P. Cruikshank, E. Dotto, Merlin, F., Poulet, F., Dalle Ore, C., Fornasier, S., De Bergh, C. (2005). "Is Sedna another Triton?". Astronomy & Astrophysics 439 (2): L1–L4. Bibcode:2005A&A...439L...1B. doi:10.1051/0004-6361:200500144.
- Hussmann, H.; Sohl, Frank; Spohn, Tilman (November 2006). "Subsurface oceans and deep interiors of medium-sized outer planet satellites and large trans-neptunian objects". Icarus 185 (1): 258–273. Bibcode:2006Icar..185..258H. doi:10.1016/j.icarus.2006.06.005.
- Trans-Neptunian Objects and Comets: Saas-Fee Advanced Course 35. Swiss Society for Astrophysics and Astronomy. Berlin: Springer. 2007. p. 86. arXiv:astro-ph/0512256v1. ISBN 3-540-71957-1.
- Lykawka, Patryk Sofia; Mukai, Tadashi (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.
- S. Alan Stern (2005). "Regarding the accretion of 2003 VB12 (Sedna) and like bodies in distant heliocentric orbits". The Astronomical Journal (Astronomical Journal) 129 (1): 526–529. arXiv:astro-ph/0404525. Bibcode:2005AJ....129..526S. doi:10.1086/426558. Retrieved 2010-08-05.
- Scott S. Sheppard, D. Jewitt (2005). "Small Bodies in the Outer Solar System" (PDF). Frank N. Bash Symposium. The University of Texas at Austin. Retrieved 2008-03-25.
- Mike Brown (2004). "Sedna and the birth of the solar system". Bulletin of the American Astronomical Society (American Astronomical Society Meeting 205) 36 (127.04): 1553. Bibcode:2004AAS...20512704B.
- "Transneptunian Object 90377 Sedna (formerly known as 2003 VB12)". The Planetary Society. Archived from the original on 25 November 2009. Retrieved 2010-01-03.
- Alessandro Morbidelli, Harold F. Levison (2004). "Scenarios for the Origin of the Orbits of the Trans-Neptunian Objects 2000 CR105 and 2003 VB12 (Sedna)". The Astronomical Journal 128 (5): 2564–2576. arXiv:astro-ph/0403358. Bibcode:2004AJ....128.2564M. doi:10.1086/424617.
- Scott J. Kenyon, Benjamin C. Bromley (2 December 2004). "Stellar encounters as the origin of distant Solar System objects in highly eccentric orbits". Nature 432 (7017): 598–602. arXiv:astro-ph/0412030. Bibcode:2004Natur.432..598K. doi:10.1038/nature03136. PMID 15577903.
- "The Challenge of Sedna". Harvard-Smithsonian Center for Astrophysics. Retrieved 2009-03-26.
- Rodney S. Gomes, John J. Matese, and Jack J. Lissauer (2006). "A distant planetary-mass solar companion may have produced distant detached objects". Icarus 184 (2): 589–601. Bibcode:2006Icar..184..589G. doi:10.1016/j.icarus.2006.05.026.
- P. S. Lykawka and T. Mukai (2008). "An Outer Planet Beyond Pluto and the Origin of the Trans-Neptunian Belt Architecture". Astronomical Journal 135 (4): 1161. arXiv:0712.2198. Bibcode:2008AJ....135.1161L. doi:10.1088/0004-6256/135/4/1161.
- Megan Schwamb (2007). Searching for Sedna's Sisters: Exploring the inner Oort cloud (PDF). Cal Tech. Retrieved 2010-08-06.
- Staff (April 25, 2006). "Evidence Mounts For Companion Star To Our Sun". SpaceDaily. Archived from the original on 7 January 2010. Retrieved November 27, 2009.
- J. G. Hills (1984). "Dynamical constraints on the mass and perihelion distance of Nemesis and the stability of its orbit". Nature 311 (5987): 636–638. Bibcode:1984Natur.311..636H. doi:10.1038/311636a0.
- = 1 "Nemesis is a myth". Max Planck Institute. 2011. Retrieved 2011-08-11.
- John J. Matese, Daniel P. Whitmire and Jack J. Lissauer (2006). "A Widebinary Solar Companion as a Possible Origin of Sedna-like Objects". Earth, Moon, and Planets 97 (3–4): 459–470. Bibcode:2005EM&P...97..459M. doi:10.1007/s11038-006-9078-6. Retrieved 2010-08-17.
- Schwamb, Megan E.; Brown, Michael E.; Rabinowitz, David L. (2009). "A Search for Distant Solar System Bodies in the Region of Sedna". The Astrophysical Journal Letters 694 (1): L45–L48. arXiv:0901.4173. Bibcode:2009ApJ...694L..45S. doi:10.1088/0004-637X/694/1/L45.
- IAU: Minor Planet Center (2008-07-02). "List of Centaurs and Scattered-Disk Objects". Central Bureau for Astronomical Telegrams, Harvard-Smithsonian Center for Astrophysics. Retrieved 2008-07-02.
- Gladman, Brett (2001). "Evidence for an Extended Scattered Disk?". Observatoire de la Cote d'Azur. Retrieved 2010-07-22.
- "The Solar System Beyond The Planets". Solar System Update : Topical and Timely Reviews in Solar System Sciences. Springer-Praxis Ed. 2006. ISBN 3-540-26056-0.
- J. L. Elliot, S. D. Kern, K. B. Clancy, Gulbis, A. A. S., Millis, R. L., Buie, M. W., Wasserman, L. H., Chiang, E. I., Jordan, A. B. (2006). "The Deep Ecliptic Survey: A Search for Kuiper Belt Objects and Centaurs. II. Dynamical Classification, the Kuiper Belt Plane, and the Core Population". The Astronomical Journal 129 (2): 1117. Bibcode:2005AJ....129.1117E. doi:10.1086/427395.
- S. Alan Stern and Harold F. Levison; Levison (2002). "Regarding the criteria for planethood and proposed planetary classification schemes" (PDF). Highlights of Astronomy 12: 205–213, as presented at the XXIVth General Assembly of the IAU–2000 [Manchester, UK, 7–18 August 2000]. Bibcode:2002HiA....12..205S.
- Michael E. Brown. "The Dwarf Planets". California Institute of Technology, Department of Geological Sciences. Archived from the original on 29 February 2008. Retrieved 2008-02-16.
- "Solar System Exploration: Multimedia: Gallery". NASA. Retrieved 2010-01-03.
- "Solar System Exploration: Missions to Dwarf Planets". NASA. Retrieved 11 November 2010.
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