There are many objects in the universe that have jets of material exploding from them. A few examples are neutron stars, black holes, quasars, and protostars. Well now we can add brown dwarfs to that list. One wonders what causes these jets and if brown dwarfs can have them what’s next?

A brown dwarf is like a failed star. It’s cool and small, with a mass range of between 10 to 90 Jupiter masses. These objects are not massive enough to start nuclear burning like normal stars. They can be hard to observe since they are so small and don’t give off nearly as much light as a normal star. There is some debate about how to distinguish a brown dwarf from a giant planet like Jupiter. There are some differences; they all have about the same radii so if the mass is higher than about 10 Jupiter masses, they have a higher density and are usually not considered a planet. Also with brown dwarfs water is always found in a gaseous state where in giant planets it condenses to ice; also planets usually have ammonia in their atmospheres while brown dwarfs do not.

Now the brown dwarf called 2MASS1207-3932 has a mass of about 24 Jupiter masses with a companion planet of about 5 Jupiter masses. This brown dwarf also has a disk around it like that seen in young stars. This is the smallest object ever observed to have a jet. The jet is moving at a speed of a few kilometers per second and stretches about 1 billion kilometers; it is also much smaller and less bright than jets seen in regular stars. Astronomers had observed jets from one other brown dwarf, so with this new discovery a pattern is emerging. Its discovery suggests that these brown dwarfs form in a similar manner to normal stars but also that outflows are driven out by objects as massive as hundreds of millions of solar masses down to Jupiter-sized objects.

Astronomers were not able to observe the jets directly. Astronomers had to use the powerful Very Large Telescope (VLT) , and only an instrument called UVES could provide the sensitivity and resolution required to “see” the jet. The results highlight the incredible level of quality of instruments available today. With ever more powerful and sensitive instruments we are observing more of these faint objects and are able to learn much more about brown dwarfs, their properties, and how they develop.

This discovery tells us more about the development of brown dwarfs, but also raises some new questions. Does this mean that giant planets also have jets that we haven’t detected yet? If not, why not? What is the cut off threshold between the two? Also, what role exactly do these jets play in the life of the brown dwarf? If not all brown dwarfs have jets, what are the resulting differences between ones that do and ones that don’t? Hopefully, as we are able to observe more of these objects with our better instruments we will learn the answers to these questions.

Saturn’s rings were first discovered by Galileo Galilei in 1610, but he was unable to identify them as rings, instead he called then “ears”. In 1655 Christiaan Huygens became the first person to identify Saturn’s “ears” as Rings. Since the discovery of the rings in 1610, there have been many theories which have attempted to describe the formation of the rings.

The most popular theory is that Saturn’s rings are only 100 million years old. These young rings would have formed by a commit that was ripped apart by Saturn’s tidal forces, or by a moon which was destroyed by a large asteroid impact. The strong evidence for this theory is that the rings are much too bright to be very old, because as time passes the rings should accumulate dust which would slowly darken the rings.

Recent simulations, based on data gathered by the Cassini mission, show that the rings might be much larger and much older than previously thought, perhaps as old as four billion years. These simulations show that the particles in the rings form clumps and are not evenly distributed particles. This could mean that there is an ongoing warfare between formation and destruction within the rings. The particles slowly clump together and a blasted apart by micro-meteors. The researchers believe that the reason for the relative brightness of the rings could be that the dust is incorporated into the centers of the clumps after reformation.

The rings consist of eleven major sub-rings. For the most part the rings have been given lettered names in the order of their discovery. The D ring is the closest to Saturn and is very faint. Voyager 1 discovered that the D ring consists of three ringlets: D73, D72, and D68. Recently Cassini has discovered that D73 has moved 200 km towards Saturn since its discovery. The C ring is about 5 meters thick and it has a mass of about 1.1×10¹⁸ kg. If viewed from above or below the ring appears transparent because 5 to 12 percent of the light perpendicular to the ring is blocked. The B ring is the thickest ring, about 5 to 15 meters. Voyager discovered “spokes” inside the B ring; these spokes were not observed again until Cassini observed them in 2007. These spokes may be seasonal phenomena, as they disappear in midsummer then reappearing around equinox, and disappearing again around midwinter. The A Ring is 10 to 30 meters thick and has a mass of about 6.2 x 10¹⁸ kg. In 2006 4 small tiny moons were discovered inside the A ring. There is now estimated to be over 1000 such moonlets inside the A ring. The F was discovered in 1979 by Pioneer 11. The ring is the most active of the rings, and is the very thin outermost ring. The ring is held together by two moons, Prometheus and Pandora. Occasionally during Prometheus’s orbit, it approaches the ring causing kinks and knots. It also steals material from the ring leaving behind a dark channel.

Besides their formation, there is still much to learn about the rings. For instance, what causes the seasonal spokes which occur inside the B ring? Why is some of the material accreted into tiny moonlets, while the rest remains as independent particles or clumps? Why has the ringlet D73 moved in towards Saturn? Whatever the answers may be, anyone who looks at Saturn through a telescope knows one thing for sure–Saturn is one of the most amazing and beautiful objects in our solar system.

Two NASA scientists have found the smallest, or lightest weight, black hole ever yet discovered. The black hole is in the binary system, XTE J1650-500, which is in the constellation Ara in the southern hemisphere. The mass of the black hole is only 3.8 solar masses. This beats the previous record holder of 6.3 solar masses. The black hole was discovered earlier as part of the binary with a normal star and was known to be lightweight but its exact weight was not known until recently with the use of a new method.

This new method uses a relationship between the black hole and the inner part of the surrounding in falling gas and material. Hot gas piles up around the black hole as it falls in and heats up giving off x-rays. The x-ray’s intensity varies in a regular pattern, called the quasi-periodic oscillation, or QPC. Astronomers discovered the congestion zone is closer to smaller black holes and therefore makes the QPC change more quickly. To measure the black hole masses, astronomers used archival data from RXTE, which has made exquisitely precise measurements of QPO frequencies in at least 15 black holes. Using this method they measured the mass of XTE J1650-500 as 3.8 solar masses with a margin of error of only half a sun.

This value is well below those measured for other standard black holes. Now there is a threshold value below which a dying star will become a neutron star instead of a black hole. It is thought to be between 1.7 to 3 solar masses. However, with this new discovery and method of detection this boundary could be in question. This value is very important for fundamental astrophysics. This is because it’s hard to know exactly what happens when a star goes supernova, when a very large amount of mass is condensed to a very small size with high density. The more details we learn about this process in particular, the more we learn about physics in general. So while the study of super massive black holes may sound more exciting, studying the smallest of black holes may be more fundamental for our understanding of physics and matter.

NASA has chosen a new mission in the Mars Exploration Program to study the Martian atmosphere. The purpose of the $485 million MAVEN mission, (Mars Atmosphere and Volatile EvolutioN), is to study the Martian Atmosphere, climate history, and potential habitability. This mission is intended to take the most detailed measurements ever recorded in the Martian atmosphere.

After the launch in 2013, MAVEN will enter an elliptical orbit from 90 to 3870 miles above the Martian surface where it will take measurements for an entire Earth year. Maven will also descend to an altitude of 80 miles above the surface where it will take detailed measurements of the upper atmosphere. After the mission is complete MAVEN will be used as a communications satellite for future rovers and landers.

The Martian atmosphere is relatively thin, with pressures ranging from .03 kPa to 1.155 kPa, and an average sea-level pressure of about .6 kPa (nearly 170 times less than that of Earth). Even though the atmosphere on Mars is 4 km taller than Earths, its Mass is nearly 206 times less than Earths. The atmosphere is composed of 95% CO₂, 3% N, 1.6% Ar, with trace amounts of O₂, H₂O, and CH₄. The atmosphere has been divided into 4 subdivisions: lower atmosphere, middle atmosphere, Upper atmosphere, and exosphere. The lower atmosphere is region that is warmed from airborne dust particles. The middle atmosphere is distinguished only by a jet stream. The upper atmosphere is characterized by very high temperatures, and the atmospheric gasses are stripped apart by the sun. The exosphere, like on Earth, is the boundary-less region where the atmosphere slowly tappers out into space.

Because Mars has the only surface observable from Earth, its climate has been studied since the 17^th century. The first up-close climate observations were made in the 60’s by the Mariner missions and the Viking missions of the 70’s. Today the Mars Global Surveyor keeps up where they left off. We know that the Martian climate has some similarities with the Earth, such as changing seasons, ice-ages, and even a sublimating south-pole which could indicate a warming climate. Unlike Earth, Mars lacks water and has a low ability to resist temperature change during a full heating/cooling cycle.

Recent Missions such as the rovers, Spirit and Opportunity, have shown that large amounts of water most likely existed on the Martian surface at one time. So with any luck, MAVEN will be able to provide some insight into where this water went, and what happened to a Martian atmosphere that was once able to support water and perhaps life. Even more importantly, MAVEN will help us understand the evolution and the eventual fate of our own atmosphere.