We now know more than one thousand extrasolar planets (exoplanets), and another two thousand exoplanet candidates. Many of the best understood ones are so-called transiting exoplanets, and many were discovered by small telescopes. I will review two currently running small telescopes projects (HATNet and HATSouth) that have altogether yielded 60 exoplanets. I will highlight some of the discoveries and recent scientific results from these projects.
A field of physics that is growing in interest worldwide that tackles such astrophysical phenomena as the source of violent space weather and the formation of stars.
The Sun emits a constant flow of particles from its surface. Mainly composed of Protons and electrons, and dragging with it magnetic fields, this Solar Wind expands outwards from the sun, interacting with planets and spacecraft alike. Since the 1960s, in situ observations have shown that the solar wind is comprised of two distinct states: slow (300550 km/s) and fast (600800 km/s). Temperature, density, and compositional variations between the two suggest different sources for the fast and slow solar wind.
Researchers at Princeton University and the U.S. Department of Energy’s (DOE) Princeton Plasma Physics Laboratory (PPPL) have launched a new center to study the volatile heliosphere — a complex and frequently violent region of space that encompasses the solar system. This region is carved out by the solar wind — charged plasma particles that constantly stream from the sun — and gives rise to space weather that can disrupt cell phone service, damage satellites and knock out power grids.
More than 1,500 researchers, including scientists from the U.S. Department of Energy’s Princeton Plasma Physics Laboratory (PPPL), have gathered in Denver, Colorado, for the 55th Annual Meeting of the American Physical Society’s (APS) Division of Plasma Physics (DPP).
Princeton astrophysicist Lyman Spitzer Jr. (1914-1997) was among the 20th Century’s most visionary scientists. His major influences range from founding the Princeton Plasma Physics Laboratory (PPPL) and its quest for fusion energy, to inspiring the development of the Hubble Space Telescope and its images of the far corners of the universe.
A new experiment called PTOLEMY (Princeton Tritium Observatory for Light, Early-Universe, Massive-Neutrino Yield) is under development at the Princeton Plasma Physics Laboratory with the goal of challenging one of the most fundamental predictions of the Big Bang – the present-day existence of relic neutrinos produced less than one second after the Big Bang. Using a gigantic sail of a single atomic layer of graphene to hold 100 grams of tritium, radio antennas capable of sensing the motion of single electrons undergoing cyclotron motion, and a massive array of cryogenic s
Was the event that occurred 13.7 billion years ago a big bang – the beginning of space and time – or a big bang bounce – a transition from contraction to expansion? This talk will explain how the two possibilities lead to very different pictures of the origin, evolution and future of the universe and how recent and near future observations may resolve which picture is correct.
Whistler-mode chorus waves were first reported in the early 1950’s and so-named due to the resemblance of their sound to a ‘rookery of birds at dawn’, when played through a loudspeaker. In the ensuing decades, as better observations and more accurate theory began to emerge, a coherent and fascinating picture began to emerge of chorus playing a key role in the dynamics of the inner magnetosphere.
More than 350 participants from around the world will gather in Plainsboro, N.J., on September 30 for the 66th Annual Gaseous Electronics Conference (GEC). The week-long event will bring together physicists from numerous plasma science disciplines for workshops, panels and poster sessions on topics ranging from basic research to uses for plasma in microchip etching, nano- material manufacturing and other technologies.
Stars do not form singly, but in groups. Within the plane of the Milky Way Galaxy, we have systems ranging in population from 100 to 10,000 members. Their origin is still poorly understood, and many basic questions remain. How do local conditions in the interstellar medium lead to one type of group rather than another? Why do the most populous and massive groups disperse after a few million years, while comparatively unimpressive systems of a few hundred stars remain intact for up to a billion years?
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