Pulsars
... • Pulsating X-ray sources / X-ray pulsators - compact objects (generally neutron stars) in binary systems Accrete matter from normal star companion (P ~ 10s, dP/dt < 0) ...
... • Pulsating X-ray sources / X-ray pulsators - compact objects (generally neutron stars) in binary systems Accrete matter from normal star companion (P ~ 10s, dP/dt < 0) ...
E N 1”=140 AU
... [2] it emits not only by scattering but also by emission lines (such as [Fe II]).
Outstanding structure is not seen.
⇒The jet is probably obscured by a circumbinary disk (if any) in the plane
perpendicular to the jet.
...
... [2] it emits not only by scattering but also by emission lines (such as [Fe II]).
The Marathon
... even need a telescope to find it! The Pleiades (M45) is visible as a compact collection of six or seven stars to the naked eye. A simple pair of binoculars will reveal dozens of beautiful blue stars. Next is the first globular cluster on our list, M79. To track down this cluster, the equivalent of 9 ...
... even need a telescope to find it! The Pleiades (M45) is visible as a compact collection of six or seven stars to the naked eye. A simple pair of binoculars will reveal dozens of beautiful blue stars. Next is the first globular cluster on our list, M79. To track down this cluster, the equivalent of 9 ...
The Hubble Redshift Distance Relation
... • Click on Field and choose another galaxy cluster. Repeat the above steps for all five clusters of galaxies. ...
... • Click on Field and choose another galaxy cluster. Repeat the above steps for all five clusters of galaxies. ...
Gilmore - Astrometry and Astrophysics in the Gaia sky
... • Physical properties, for example: – clean Hertzsprung-Russell sequences throughout the Galaxy – solar neighbourhood mass function and luminosity function e.g. white dwarfs (~200,000) and brown dwarfs (~50,000) – initial mass and luminosity functions in star forming regions – luminosity function fo ...
... • Physical properties, for example: – clean Hertzsprung-Russell sequences throughout the Galaxy – solar neighbourhood mass function and luminosity function e.g. white dwarfs (~200,000) and brown dwarfs (~50,000) – initial mass and luminosity functions in star forming regions – luminosity function fo ...
sBzKs
... E(B-V)～0.40, average SFR ～ 190 Mo/yr, typical stellar mass ～1011 Mo, and ～solar metallicity. The high SFRs, large masses and high metallicities of sBzKs suggest that these z～2 star forming galaxies are the precursors of z=1 passive EROs and z=0 early-type galaxies. ...
... E(B-V)～0.40, average SFR ～ 190 Mo/yr, typical stellar mass ～1011 Mo, and ～solar metallicity. The high SFRs, large masses and high metallicities of sBzKs suggest that these z～2 star forming galaxies are the precursors of z=1 passive EROs and z=0 early-type galaxies. ...
An Introduction To Parallax
... Even the nearest star, Alpha Centauri, is more than 200,000 times further away than the diameter of the Earth’s orbit. This means that the shift in angle we observe in Alpha Centauri is less than 1 second of arc, or less than the thickness of a hair seen across a large rooma . It was not until the m ...
... Even the nearest star, Alpha Centauri, is more than 200,000 times further away than the diameter of the Earth’s orbit. This means that the shift in angle we observe in Alpha Centauri is less than 1 second of arc, or less than the thickness of a hair seen across a large rooma . It was not until the m ...
Magnitude scale theory
... In our example if A appears to the observer to be brighter than B, and if we use m A to be the absolute magnitude (M) then its apparent magnitude (mB) is less and so its distance must be more than 10 pc. ...
... In our example if A appears to the observer to be brighter than B, and if we use m A to be the absolute magnitude (M) then its apparent magnitude (mB) is less and so its distance must be more than 10 pc. ...
Distances to the Hyades Cluster
... To find the distance to the Hyades star cluster using the convergent point method; to recognize the uncertainties in using this method; to summarize the significant results obtained by the Hipparchos satellite and what these results mean for the distance scale of the Universe. Background and Theory ...
... To find the distance to the Hyades star cluster using the convergent point method; to recognize the uncertainties in using this method; to summarize the significant results obtained by the Hipparchos satellite and what these results mean for the distance scale of the Universe. Background and Theory ...
Astro 27 Solar System Formation and ExoPlanets Slide Show
... nebula while it was hot enough (>1600K) for CAI material to not yet have solidified. • Gritschneder et.al. 2011 hydro simulations show a massive star supernova (type II SN) within a Giant Molecular Cloud, and 5pc away from a reasonble overdensity, would both compress the overdensity cloud to initiat ...
... nebula while it was hot enough (>1600K) for CAI material to not yet have solidified. • Gritschneder et.al. 2011 hydro simulations show a massive star supernova (type II SN) within a Giant Molecular Cloud, and 5pc away from a reasonble overdensity, would both compress the overdensity cloud to initiat ...
- UCL Discovery
... aim to model the interstellar medium (ISM), star formation and stellar feedback in a galaxy. As dwarf galaxies are physically small, the physical resolution is higher if the simulations use a similar number of resolution elements to simulations of larger galaxies, like the Milky Way. Mori et al. (19 ...
... aim to model the interstellar medium (ISM), star formation and stellar feedback in a galaxy. As dwarf galaxies are physically small, the physical resolution is higher if the simulations use a similar number of resolution elements to simulations of larger galaxies, like the Milky Way. Mori et al. (19 ...
ABC`s of the Sky - Northern Stars Planetarium
... Stars Stars are huge balls of hydrogen gas that shine with light and heat because of powerful nuclear explosions that continually explode in their centers. The Sun is the closest star. Other stars are just as big as the Sun, they only look small because they are very very far away. Telescope A teles ...
... Stars Stars are huge balls of hydrogen gas that shine with light and heat because of powerful nuclear explosions that continually explode in their centers. The Sun is the closest star. Other stars are just as big as the Sun, they only look small because they are very very far away. Telescope A teles ...
Population synthesis of Be/white dwarf binaries in the Galaxy
... Abstract. Using the “Scenario Machine” (a numerical code that models the evolution of large ensembles of binary systems) we study the number and physical properties of binary Be stars with white dwarfs taking account of the compact object cooling and we discuss the ways of their formation. In our ca ...
... Abstract. Using the “Scenario Machine” (a numerical code that models the evolution of large ensembles of binary systems) we study the number and physical properties of binary Be stars with white dwarfs taking account of the compact object cooling and we discuss the ways of their formation. In our ca ...
hydrogen deficient stars and related objects
... the white dwarfs as some of these stars are no doubt genetically linked to our helium stars. The central and most startling problem in the field of helium stars, something which has puzzled us from the very beginning, is how extreme helium stars are formed and how a star of one solar mass may get ri ...
... the white dwarfs as some of these stars are no doubt genetically linked to our helium stars. The central and most startling problem in the field of helium stars, something which has puzzled us from the very beginning, is how extreme helium stars are formed and how a star of one solar mass may get ri ...
Collapse of an unstable Neutron Star to a Black Hole
... star merger process a new supramassive or hypermassive neutron star is formed, which could be stable for longer times or collapse almost immediately to a black hole. During this process a short gamma ray burst is emitted, releasing in less than one second the energy emitted by our Galaxy over one ye ...
... star merger process a new supramassive or hypermassive neutron star is formed, which could be stable for longer times or collapse almost immediately to a black hole. During this process a short gamma ray burst is emitted, releasing in less than one second the energy emitted by our Galaxy over one ye ...
EXPERIMENTAL TESTS OF GENERAL RELATIVITY
... If the “lens”(i.e. the object whose presence causes the light rays from the source to be deflected on their way to the observer) is small (star, planet), then the separation between the images of the sources is too small to be resolved, and what the observer sees is an overall increase in the bright ...
... If the “lens”(i.e. the object whose presence causes the light rays from the source to be deflected on their way to the observer) is small (star, planet), then the separation between the images of the sources is too small to be resolved, and what the observer sees is an overall increase in the bright ...
Day-1
... ASTR 2010: Problems in Planetary Astronomy meets Wednesdays at 1600 (E118). It is a onehour class that only meets once a week. We will do some of the problems from the back of the chapters that involve math as well as supplemental problems. The math level is basic algebra. If you are interested, see ...
... ASTR 2010: Problems in Planetary Astronomy meets Wednesdays at 1600 (E118). It is a onehour class that only meets once a week. We will do some of the problems from the back of the chapters that involve math as well as supplemental problems. The math level is basic algebra. If you are interested, see ...
PSC100 Summary Chapters 1 to Chapter 9
... frequency components and spectra elements of these signals. If we do, we can achieve phenomenal insights into the complex structure and evolution of things that are billions of light years away from us in space and which we will never be able to visit or experiment on first hand. When we study the u ...
... frequency components and spectra elements of these signals. If we do, we can achieve phenomenal insights into the complex structure and evolution of things that are billions of light years away from us in space and which we will never be able to visit or experiment on first hand. When we study the u ...
White Dwarf Stars - Stellar Physics Department
... H for magnetic white dwarfs that do show any detectable polarization. P for polarized magnetic white dwarfs. V for variable white dwarfs. And finally to complete the classification, a temperature index can follow their spectral classification. This index is defined as θ = 50400/Teff . Therefore, a w ...
... H for magnetic white dwarfs that do show any detectable polarization. P for polarized magnetic white dwarfs. V for variable white dwarfs. And finally to complete the classification, a temperature index can follow their spectral classification. This index is defined as θ = 50400/Teff . Therefore, a w ...
PODEX – PhOtometric Data EXtractor
... curve. A light curve with a high D–value and/or a high variance has low weight for the reference light curve. Clicking the Calc Va-Cp button, the reference light curve is determined and subtracted from the light curve of star #1. The resulting relative (or absolute, if the offset cor. option is used ...
... curve. A light curve with a high D–value and/or a high variance has low weight for the reference light curve. Clicking the Calc Va-Cp button, the reference light curve is determined and subtracted from the light curve of star #1. The resulting relative (or absolute, if the offset cor. option is used ...
Hot HB stars in globular clusters
... of about 4 . 7, which places it at the very faint blue end of the EHB as seen in the colour-magnitude diagram of NGC 6752. F2-2 may even be hotter than any EHB star in NGC 6752. From its proximity to the helium main sequence in Fig. 4 and 5 it might be tempting to regard F2-2 as a naked helium core, ...
... of about 4 . 7, which places it at the very faint blue end of the EHB as seen in the colour-magnitude diagram of NGC 6752. F2-2 may even be hotter than any EHB star in NGC 6752. From its proximity to the helium main sequence in Fig. 4 and 5 it might be tempting to regard F2-2 as a naked helium core, ...
Energy in The Universe - Physics Department, Princeton University
... is the size hangup. A na'ive person look ing at the cosmos has the impression that the whole thing is extravagantly, even irrelevantly, large. This extravagant size is our primary protection against a varie ty of catastrophes. If a volume of space is filled with matter with an average densi ty d, ...
... is the size hangup. A na'ive person look ing at the cosmos has the impression that the whole thing is extravagantly, even irrelevantly, large. This extravagant size is our primary protection against a varie ty of catastrophes. If a volume of space is filled with matter with an average densi ty d, ...
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.