THE GALACTIC GAZETTE The Astronomical Society of Southern New England Next Meeting
... Cataclysmics, also known as dwarf novae, are binary stars in close orbit about one another. One of them is Sunlike, the other a compact white dwarf star with an appetite. Their embrace is so tight — 100,000 miles for SS Cygni according to some estimates — that the dwarf's powerful gravity strips mat ...
... Cataclysmics, also known as dwarf novae, are binary stars in close orbit about one another. One of them is Sunlike, the other a compact white dwarf star with an appetite. Their embrace is so tight — 100,000 miles for SS Cygni according to some estimates — that the dwarf's powerful gravity strips mat ...
February 2004
... Mars is still in the evening sky in the north west, perhaps almost forgotten after its showing last August, it could be mistaken for a star like Betelgeuse, (it nearly was!) but it is still in a part of the sky where there are not many other bright objects. It showed a small disc in Michael’s 3 inch ...
... Mars is still in the evening sky in the north west, perhaps almost forgotten after its showing last August, it could be mistaken for a star like Betelgeuse, (it nearly was!) but it is still in a part of the sky where there are not many other bright objects. It showed a small disc in Michael’s 3 inch ...
a kiloparsec-scale nuclear stellar disk in the milky way
... forming a stellar nuclear disk (Cole et al. 2014), to derive the kinematic signatures of such a disk. We use these to guide our interpretation of the APOGEE Data Release 12 (Alam et al. 2015) stellar velocity data for the inner MW. While the simulation was not designed to match the MW, Cole et al. ( ...
... forming a stellar nuclear disk (Cole et al. 2014), to derive the kinematic signatures of such a disk. We use these to guide our interpretation of the APOGEE Data Release 12 (Alam et al. 2015) stellar velocity data for the inner MW. While the simulation was not designed to match the MW, Cole et al. ( ...
Online version of poster
... Physical state of the collapsing core. The situation is shown just prior to the formation of the first sink particle. (a) Temperature; (b) free electron fraction; (c) molecular hydrogen fraction; and (d) adiabatic exponent γad vs. density. The gas that collapses into the minihalo is heated adiabatic ...
... Physical state of the collapsing core. The situation is shown just prior to the formation of the first sink particle. (a) Temperature; (b) free electron fraction; (c) molecular hydrogen fraction; and (d) adiabatic exponent γad vs. density. The gas that collapses into the minihalo is heated adiabatic ...
featured in the Arizona Daily Star
... piece of a star and study it in the laboratory. That’s what I do — I study pieces of ancient stardust. But instead of using a telescope, I use a microscope to look for stardust inside meteorites. Over their lifetimes, stars shed matter that can condense into solid mineral grains — stardust — if cond ...
... piece of a star and study it in the laboratory. That’s what I do — I study pieces of ancient stardust. But instead of using a telescope, I use a microscope to look for stardust inside meteorites. Over their lifetimes, stars shed matter that can condense into solid mineral grains — stardust — if cond ...
Document
... gamma ray bursts have been found to be associated with the deaths of very large stars. The favored models for these is the “core collapse supernova,” where the massive core of the star collapses into a black hole and black hole accretion powers a luminous jet. Despite numerous observations, many of ...
... gamma ray bursts have been found to be associated with the deaths of very large stars. The favored models for these is the “core collapse supernova,” where the massive core of the star collapses into a black hole and black hole accretion powers a luminous jet. Despite numerous observations, many of ...
planetary standard model
... The necessary observations may not be possible: stars young enough to have planets migrating through protoplanetary disks are still surrounded by dust, and their light flickers, making it extremely unlikely that current methods will be able to pick out the dimming caused by a transiting planet. The ...
... The necessary observations may not be possible: stars young enough to have planets migrating through protoplanetary disks are still surrounded by dust, and their light flickers, making it extremely unlikely that current methods will be able to pick out the dimming caused by a transiting planet. The ...
here - Canadian Institute for Theoretical Astrophysics
... The necessary observations may not be possible: stars young enough to have planets migrating through protoplanetary disks are still surrounded by dust, and their light flickers, making it extremely unlikely that current methods will be able to pick out the dimming caused by a transiting planet. The ...
... The necessary observations may not be possible: stars young enough to have planets migrating through protoplanetary disks are still surrounded by dust, and their light flickers, making it extremely unlikely that current methods will be able to pick out the dimming caused by a transiting planet. The ...
Life Stages of High
... • After core helium fusion stops, He fuses into carbon in a shell around the carbon core, and H fuses to He in a shell around the helium layer. • This double-shell-burning stage never reaches equilibrium—the fusion rate periodically spikes upward in a series of thermal pulses. • With each spike, con ...
... • After core helium fusion stops, He fuses into carbon in a shell around the carbon core, and H fuses to He in a shell around the helium layer. • This double-shell-burning stage never reaches equilibrium—the fusion rate periodically spikes upward in a series of thermal pulses. • With each spike, con ...
b. false - UW Canvas
... good representation of how stars “work,” we would conclude that a. the hotter the star is, the more luminous it is, and the brighter the colors will be overall. b. the cooler the star, the less luminous it is; the brighter part of the spectrum will be toward longer wavelengths. c. the luminosity of ...
... good representation of how stars “work,” we would conclude that a. the hotter the star is, the more luminous it is, and the brighter the colors will be overall. b. the cooler the star, the less luminous it is; the brighter part of the spectrum will be toward longer wavelengths. c. the luminosity of ...
The Circumstellar Medium of Massive Stars in Motion
... magnetohydrodynamics of the photoionised H II region around the nearby runaway O star ζ Oph. Finally, we have calculated a grid of models of bow shocks around main sequence and evolved massive stars that has general application to many observed bow shocks, and which forms the basis of future work to ...
... magnetohydrodynamics of the photoionised H II region around the nearby runaway O star ζ Oph. Finally, we have calculated a grid of models of bow shocks around main sequence and evolved massive stars that has general application to many observed bow shocks, and which forms the basis of future work to ...
Constellations and Light Pollution
... own world was formed. Yet, after traveling countless light years, the light from these objects can be lost at the end of its journey in the glare of our own sky. Space-based telescopes, such as the Hubble Space Telescope, offer one way around the problem. However, large telescopes on Earth will alwa ...
... own world was formed. Yet, after traveling countless light years, the light from these objects can be lost at the end of its journey in the glare of our own sky. Space-based telescopes, such as the Hubble Space Telescope, offer one way around the problem. However, large telescopes on Earth will alwa ...
My power point presentation on spectroscopy of stars (ppt file)
... • We can hardly see any surface details from the solar system, except for our own Sun • The interior of a star is even more hidden than the surface layers • Essentially the only information a star sends to us is its electromagnetic radiation • Can we dissect the radiation from a star to find out any ...
... • We can hardly see any surface details from the solar system, except for our own Sun • The interior of a star is even more hidden than the surface layers • Essentially the only information a star sends to us is its electromagnetic radiation • Can we dissect the radiation from a star to find out any ...
PowerPoint Presentation - Neutron stars, pulsars and black
... than 100 times per second (the first was spinning 640 times per second) threw the field for a loop. When some millisecond pulsars were discovered in old star clusters it was even more confusing. • Eventually it was determined that all millisecond pulsars were in close binary systems and were `spun u ...
... than 100 times per second (the first was spinning 640 times per second) threw the field for a loop. When some millisecond pulsars were discovered in old star clusters it was even more confusing. • Eventually it was determined that all millisecond pulsars were in close binary systems and were `spun u ...
get ready for rtmc may 26-28th!
... burning. Theory said that both members of such a binary pair would have formed at the same time, and the smaller one would have (continued on page 8) ...
... burning. Theory said that both members of such a binary pair would have formed at the same time, and the smaller one would have (continued on page 8) ...
L12-no equations
... Spectrum of Crab pulsar is nonthermal. Suggestive of synchrotron radiation - relativistic charged particles emit radiation dependent on particle energy. Charged particles (e-) accelerated along magnetic field lines, radiation is beamed in the the acceleration direction. If axes are not aligned, lead ...
... Spectrum of Crab pulsar is nonthermal. Suggestive of synchrotron radiation - relativistic charged particles emit radiation dependent on particle energy. Charged particles (e-) accelerated along magnetic field lines, radiation is beamed in the the acceleration direction. If axes are not aligned, lead ...
Document
... Main Sequence stars: H burning in the core, synthesizing light elements Heavier elements form in the later stages, after H in the core is exhausted and core contracts, central T rises to ignite “triple-” reaction 3 He4 --> C12 Which stars can ignite He? If they cannot, what happens during the contr ...
... Main Sequence stars: H burning in the core, synthesizing light elements Heavier elements form in the later stages, after H in the core is exhausted and core contracts, central T rises to ignite “triple-” reaction 3 He4 --> C12 Which stars can ignite He? If they cannot, what happens during the contr ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.