Research finds numerous unknown jets from young stars and planetary nebulae

July 31, 2014, University of Kent
The area shown here was part of the very first image taken for the UWISH2 survey. It shows on the top a region of massive star formation (called G35.2N) with two spectacular jets. On the bottom an intermediate mass young stellar cluster (Mercer14) can be seen. Several jets are visible in its vicinity, as well as a region of photo-ionized material surrounding a young massive star. Credit: University of Kent

For many years astronomers have known that young 'protostars' drive supersonic jets of gas from their north and south poles. However, this is the first time that so many of them have been detected at once.

The results come from a five year survey undertaken with the UK Infra-Red Telescope and are expected to prompt significant changes in the understanding of the planetary nebulae population in the Galaxy, as well as the properties of ejected from young forming stars.

By examining images of excited at , scientists have been able to see through the gas and dust in the Milky Way in order to observe more distant targets. These targets are normally hidden from view and many of them have never been seen before.

The entire survey area covers approximately 1450 times the size of the full moon, or the equivalent of a 95 GigaPixel image. The survey reveals jets from protostars and planetary nebulae, as well as , the illuminated edges of vast clouds of gas and dust, and the warm regions that envelope massive stars and their associated clusters of smaller stars.

Based on current estimates using these data, the project expects to identify about 1000 unique jets from young stars - at least 90% of these are new discoveries – as well as 300 planetary nebulae, with almost half of them unknown.

This is a text-book example of triggered star formation. There is the outline of a molecular cloud, which is illuminated by ionizing radiation of massive stars situated off the bottom of the image. The radiation pressure has compressed the cloud and started the process of star formation. The forming stars can be identified by reflection nebulae surrounding them, or by their jets. Models of the process of triggered star formation predict an age gradient of the forming stars with younger objects further inside, away from the source of the ionizing radiation. The object shown here is a prime example that confirms this scenario with reflection nebulae ranging in colors from blue, near the tip of the molecular cloud, to green and yellow further inside. The color change towards red indicates the objects are further embedded in their parental cloud core and thus younger. The youngest object is completely invisible even at these infrared wavelengths, and can only by identified by the jet it is launching (top of image). Credit: University of Kent

Dr Dirk Froebrich of the University's Centre for Planetary Science said: 'These discoveries are very exciting. We will ultimately have much better statistics, meaning we will be able to investigate the physical mechanisms that determine the jet lengths, as well as their power. This will bring us much closer to answering some of the fundamental questions of star formation: How are these jets launched and how much energy, mass and momentum do they feed back into the surrounding interstellar medium.'

To mark the 5th anniversary of the start of the observations of the survey on 27 August, the project has released a number of images taken with the UK Infra-Red Telescope, based in Hawaii and used for the research.

MEDIA NOTE: Images available to download below.

This image shows a field that contains a newly discovered photogenic planetary nebulae. Internally dubbed by the research team as the "Jelly-Fish PN" it shows an almost circular ring of emission from molecular hydrogen with a variety of structure in the ring itself and inside. The central ionizing source responsible for the radiation is a white dwarf, which is too faint at the near infrared wavelengths to be visible in the image. Credit: University of Kent

The project has been led by Dr Dirk Froebrich from the Centre for Planetary Sciences at the University of Kent, in collaboration with Dr Chris J. Davis from the Astrophysics Research Institute at Liverpool John Moores University.

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1.7 / 5 (6) Jul 31, 2014
The Electric Universe is alive and well.
But they'll probably run their delusional gravity based computer simulations to confuse everyone a little more.
1.7 / 5 (6) Jul 31, 2014

Here ya go. Read up buddy.
5 / 5 (1) Aug 01, 2014
According to my computations, electric charge would have very little influence on gravitating heavy bodies like stars and planets, but would have a significant influence on small bodies like binary asteroids and small clumps of gas. Take an electric potential of 1 kV that would charge said bodies at surface. Then the ratio between electric acceleration and gravitational acceleration would be about 1.7 for binary orbiting asteroids of about 1 meter radius and 1 700 000 for binary self-gravitating clumps of gas 1 meter in radius. This can be checked inside the Solar System, where there may be binary asteroids of that size. Their orbiting speed should be very different from that given by their mutual gravity alone.

Simply having the Solar System charged at constant voltage (or a spread of voltages) of 1kV magnitude will have significant influence on such small systems. Even breaking a charged body into 2 parts and setting them into self-orbiting trajectories will show that difference.
2.7 / 5 (7) Aug 01, 2014
but still don't appear in these images with their theorized surface temperature and emission spectrum

Because the red in the images is narrow band. Just like if you look at any other nebula with a narrow band filter the nebula is much more pronounced than the stars, unlike the stars it emits lines not continuum. White dwarfs are naturally dim anyway due to their small size, they can ionize because they emit much of their light in the ultraviolet. This is combined with the narrow band imaging to mean it is very very dim.

I'd like to see your calculation, I certainly won't take your word for it.

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