Showing posts with label Dawn Probe. Show all posts
Showing posts with label Dawn Probe. Show all posts

Sunday, 23 March 2014

The origin of Ceres.

Ceres is the largest body in the Main Asteroid Belt, comprising roughly 1/3 of all the mass of the belt. It has the designation (1) Ceres, indicating that it was the first asteroid discovered  (by Giuseppe Piazzi in 1801), but has recently been declared to be a Dwarf Planet, due to its large size, a designation that places it in the same class of bodies as the Trans-Neptunian Objects Pluto, Haumea, Eris and Makemake. As such it is the subject of considerable interest to planetary scientists, and was one of two bodies chosen to be visited by NASA’s Dawn Mission, along with (4) Vesta, the second largest body in the Main Asteroid Belt.

The results of the Dawn Mission have revealed striking differences between the two bodies, with Vesta having a subspherical shape and a cratered, volcanic surface (much as was expected from an asteroid), but Ceres has an (unexpected) smooth, icy surface and a more-or-less spherical shape. Moreover Ceres is considerably less dense than Vesta (at 2.077 g cm¯³ compared to 3.456 g cm¯³ for Vesta), suggesting that the ice forms a significant proportion of its mass, rather than simply being a thin surface layer, and several points of cryovolcanic activity, where water vapour is being released from the surface at a rate of about 6 kg s¯¹ have been discovered.

The surface of Ceres. NASA/JPL/Dawn Mission.

The surface of Vesta. NASA/JPL/Dawn Mission.

In a paper published on the arXiv online database at Cornell University Library on 20 March 2014, Yury Rogozin of the VEDA LLC in Moscow speculates that Ceres may have begun it existence not as a Main Asteroid Belt object, but as the moon of a now destroyed planet beyond the snowline of the early Solar System (the snowline being the point beyond which it was cool enough for water-ice to form, not possible within the inner Solar System due to the heat from the early Sun), and that it may have reached its current position by interaction with the gravity of the giant planet Jupiter.

Rogozin cites as evidence of this the theory that the planets Mercury and Mars may also have started out as the satellites of larger bodies (a theory which is not currently widely supported among planetary scientists). That theory goes something like this: Mercury and Mars are significantly smaller than the other two rocky planets, Earth and Venus, but are of comparable size to the larger moons of the Solar System, such as Earth’s Moon, the four Galilean moons of Jupiter, Titan etc. Furthermore Mercury and Mars have greater orbital eccentricities than any other planets in the Solar System (i.e. their distance from the Sun varies more than that of other planets). This theory speculates that Mercury is an escaped moon of Venus, and that Mars was formerly a moon of the planet Phaeton, which existed within what is now the Main Asteroid Belt, but which was destroyed by the gravitational influence of Jupiter early in the history of the Solar System.

Rogozin reasons that Mercury is in a 5:2 orbital resonance with Venus (i.e. it completes five orbits four every two orbits of Venus), and Mars is in a 5:2 resonance with the (hypothetical) orbit of the former planet Phaeton. Therefore Ceres could be in a 5:2 orbital resonance with another now destroyed planet, which Rogozin names Yurus, which would therefore have had a semi major axis (average orbital distance from the Sun) of 5.0951 AU (i.e. 5.0951 times the distance at which the Earth orbits the Sun), and an orbital period of 11.5 years.

The orbit of Ceres. JPL Small Body Database Browser.

Rogozin further suggests that the destruction of a large icy planet in such an orbit might account for the large volumes of water present on Earth and now believed to formerly have been present on Mars, both planets which are thought to have formed within the snow line, and which might therefore be expected to be largely waterless.

While the idea that Ceres may have formed beyond the early Solar System’s snow line has some merit, the existence of the planet Yurus seems highly speculative. The separation of Mercury and Mars from the other rocky planets as moon-like objects is not widely supported among planetary scientists. While Mercury is of similar size to several moons, Mars is in fact of intermediate size between these bodies and the larger rocky planets, and studies of other stellar systems have revealed a variety of rocky planets of intermediate sizes. Therefore most planetary scientists now either regard the four rocky planets as a discreet group, or use a grouping of ‘rocky worlds’ which includes the four planets, plus the fifteen largest moons in the Solar System.

The destruction of a large icy planet at a distance of 5.0951 AU from the Sun would be easy to explain, due to the closeness of such a planet to the orbit of Jupiter, a body which will excerpt considerable tidal stress on any nearby body, which has a semi major axis of 5.204267 AU, and which at its perihelion (the closest point in its orbit to the Sun) is only 4.950429 AU from the Sun; however the formation of a planet in such a position would require considerable explanation for the same reason, and explanation that Rogozin does not provide. The presence of water on Earth and Mars is more usually explained by hypothesizing a large number of comet impacts during the early history of the Solar System (the Early Bombardment Theory); comets that are thought to have formed in the outer parts of the Solar System, safely beyond the snow line.

Furthermore the speed at which a body orbits the Sun, and its distance from the Sun, are usually thought to be connected, with bodies that accelerate or slow in their orbits correspondingly moving towards or away from the Sun. Orbital resonances are usually explained by the exchange of inertia between bodies. A faster body approaching a slower body in a similar orbit will impart some of its inertia to it via tidal exchange, causing the slower body to accelerate and the faster body to slow down. The bodies will continue to exchange energy each time they pass, with one body accelerating and the other slowing each time they pass, until they reach a stable resonance. 

Several bodies within the Solar System (and in other known planetary systems) are in such resonances, most notably the three inner Galilean moons of Jupiter, which have a 4:2:1 orbital resonance. Where two bodies are in similar orbits but cannot reach a stable resonance, it is predicted that one of them will be expelled into a quite different orbit. Thus an origin of Ceres as a fifth large moon of Jupiter, unable to form a stable resonance with the other four Galilean moons and therefore expelled from the Jovian system by tidal forces, would present an alternative theory for the origin of Ceres (and an equally hypothetical one). The presence of an icy body in the Jovian system requires no explanation, as Jupiter is beyond the snow line, and has several icy moons.

The icy surface of the Jovian moon Europa. NASA/Galileo.


Follow Sciency Thoughts on Facebook.

Friday, 13 April 2012

Images of Vesta.

Vesta is the second largest object in the main asteroid belt (after Ceres), with a mass of 259 million gigatonnes and an average diameter of 530 km. Vesta orbits the sun every 3.63 years, at an average distance of 2.36 AU, (2.36 times the distance at which the Earth orbits the Sun).

The South Pole of Vesta, imaged by Dawn on 16 September 2011.NASA/JPL/CalTech.

The Dawn Space Probe has been orbiting Vesta since July 2011, gathering data and beaming images back to Earth, which has enabled scientists to build up a map of the surface of the asteroid, and start to understand the processes shaping its surface.

Quadrangle map of Vesta. NASA/JPL/CalTech.

The rim of a crater near Vesta's equator, in an area known as the Numisia Quadrangle. The crater is apparently quite recent, with signs of collapse around the rim. The light colour implies minerals that have recently (in geological terms) been exposed, over time the Sun's radiation will darken them. Taken on 18 December 2011 from a distance of 272 km. NASA/JPL/CalTech.

Impact crater in the Sextilia Quadrangle of Vesta’s southern hemisphere, surrounded by a number of dark marks. These are thought to be the result of the impact of a carbon rich meteor. Image taken on 8 January 2012 from a distance of 210 km. NASA/JPL/CalTech.

Rim of Marcia Crater in Vesta's northern hemisphere. Mozaic made from two images taken on 21 December 2011 and 5 January 2012 from distances of 130 and 210 km respectively. NASA/JPL/CalTech.

The wider area around Marcia Crater, showing darker patches caused by ejecta from the impact event. Mozaic made up of a number of images taken between 11 and 16 October 2011, from an average distance of 680 km. NASA/JPL/CalTech.

Part of the wall of the Rheasilvia Impact Basin, a 500 km diameter feature that dominates Vesta's southern hemisphere. Taken on 27 December 2011 from a distance of 210 km. NASA/JPL/CalTech.

Young crater within the Rheasilvia Impact Basin, about 15 km in diameter. Image taken on 21 December 2011 from a distance of 210 km. NASA/JPL/CalTech.

Part of the interior of the Rheasilvia Impact Basin, showing signs of rocks having flowed, as a result of an impact. Image taken on 18 December 2011 from a distance of 210 km. NASA/JPL/CalTech.

Severina Crater in the Rheasilvia Quadrangle. NASA/JPL/CalTech.

Ancient crater in the Oppia Quadrangle. The rim is degraded by a large number of smaller, more recent events. Image taken from a distance of 272 km. NASA/JPL/CalTech.


Follow Sciency Thoughts on Facebook.

Saturday, 24 December 2011

The structure of Vesta.

NASA's Dawn Probe moved into orbit around the asteroid Vesta on 16 July this year (2011) and has been beaming information back to Earth ever since. A picture has emerged of an oblate spheroid (squashed ball-shaped) world measuring 578 × 458 km, with a surface dominated by a large crater 460 km in diameter (Rheasilvia) at the southern pole; a series of grooves around the centre of the asteroid appear to be stress structures caused by the Rheasilvia impact.

A false-colour image of the surface of Vesta, centered on the Rheasilvia Crater.

This month NASA scientists attending the Fall Meeting of the American Geophysical Union report the discovery of of a metallic core and magnetic field in Vesta. This allows some interesting inferences about the history of Vesta to be made. In order to have assumed a spherical shape with a differentiated metal core Vesta must have taken a considerable time to cool, far longer than can be explained by its current size. The most likely explanation for this is that Vesta lost an appreciable amount of it's mass as a result of the Rheasilvia impact.

Vesta is currently designated as an Asteroid, rather than a Dwarf Planet, a body large enough to assume a spherical structure due to its own gravity, as it was not thought to be massive enough to achieve this, but Vesta is clearly roughly spherical, so either our theories on how massive a body must be to assume a spherical shape are wrong, or Vesta has lost some mass since it formed, something which the Rheasilvia impact can explain. It is likely that Vesta will be redesignated as a Dwarf Planet in the near future.

A map of the magnetic field of Vesta; like the surface this clearly shows the effects of the Rheasilvia impact.

The Dawn Probe is due to leave Vesta in July 2012 and move on to Ceres, which it will reach in February 2015. Ceres was formerly considered to be the largest asteroid in the Solar System; though since the introduction of the Dwarf Planet classification it has been considered the smallest Dwarf Planet, with Vesta, formerly the second largest asteroid promoted to largest asteroid.

Tuesday, 2 August 2011

The surface of Vesta.

A week after NASA/JPL's Dawn Space Probe moved into orbit around the asteroid Vesta images of the hole of the surface have been released. Vesta is the second largest object in the Asteroid Belt and has a surface area of 883 000 km², twice that of California or 42 times that of Wales. It shows considerable variation over its surface.

Animation of the Surface of Vesta.
There is a higher resolution version on the Dawn website here.

Much of the south of the asteroid is smooth, while northern part of Vesta is heavily pitted, the result of many small impacts. This implies the northern surface is older than the southern; the most likely scenario is that both hemispheres were pitted heavily by impacts early in the solar system's history (though still over a very long period of time), and that the southern hemisphere was then resurfaced by a single large impact.

Overlapping craters nicknamed 'The Snowman'
in the Northern Hemisphere of Vesta.

The equatorial region of Vesta show heavy grooving, which is unexpected. Similar grooves are also seen on the Martian moon, Phobos, where they are attributed to repeated impacts by debris in the same orbit as the moon, repeatedly striking from the same direction. The Russian Phobos-Grunt mission is due to visit the moon and collect samples in 2013, which should vastly improve our understanding of Phobos' history.

Grooves on the surface of Phobos.

This is surprising on Vesta as it occupies a more sparse area of space; our current understanding implies the Asteroid Belt to be made up of scattered, remote objects. The grooving implies that early in the Solar System's history the Asteroid Belt may have been more densely packed.

The Dawn Probe should remain in orbit about Vesta for a year, during which time it should gather considerable information about the asteroid's structure and mineralogy. After this it will move on to Ceres, the largest object in the Asteroid Belt.

See also Visiting Vesta, 2010 TK₇, Earth's Trojan Asteroid and Asteroid 2011MD.

Monday, 18 July 2011

Visiting Vesta

On the 16th of July 2011 the NASA space probe Dawn moved into orbit around the asteroid Vesta, 188 million km from the Earth, where it will remain for the next year.

An artist's impression of the Dawn space probe.

Vesta was discovered by German astronomer Heinrich Wilhelm Olbers in 1807, the forth object to be discovered in what we now call the Asteroid Belt. It has a diameter of about 530 km and is the second most massive object in the belt, potentially containing 9% of the total mass of the Asteroid Belt. Vesta orbits at a distance of 2.5 AU (i.e. 2.5 times as far from the sun as the Earth is). It is roughly spherical in shape, but is slightly to small to be considered a dwarf planet. Scientists believe that its shape indicates that it underwent at least partial melting early in its history, due to the decay of radioactive elements in its core - the same process that keeps the interior of the Earth molten. Vesta has a number of prominent craters, most notably the 460 km diameter (80% of that of the whole asteroid) at it's south pole.

Vesta.

The Dawn probe is designed to shed light on the early development of the solar system by examining Vesta and Ceres, the two largest objects in the asteroid belt, both of which are thought to be relatively unchanged since their formation, early in the history of the system. The Dawn probe is powered by an ion drive, a new technology which has the potential to vastly improve our ability to explore the solar system. The drive uses two large solar panels to ionize Xenon gas, which is then fired through an electric field creating thrust. This generates less thrust than a conventional rocket engine, but is much smaller and can maintain thrust for much longer, making it a far more efficient system as long as you do not wish to get anywhere in a hurry.

A diagrammatic representation of the ion drive which powers the Dawn probe.

See also Asteroid 2011MD.