Chapter 1: Introduction to Wide
... achieved quickly. The concepts and techniques learned in wide-field work are critical to success in later, more complex astrophoto work. Basic widefield astrophotography is often regarded as the first step in a learning process that eventually leads to deep-sky photography. However, wide-field astro ...
... achieved quickly. The concepts and techniques learned in wide-field work are critical to success in later, more complex astrophoto work. Basic widefield astrophotography is often regarded as the first step in a learning process that eventually leads to deep-sky photography. However, wide-field astro ...
Type II Supernovae
... An observer in the orbital plane has θ = π/2 and h× = 0. The observed frequency of gravitational waves is ν = Ω/π. The intensity of gravitational waves decreases as 1/r. Consider two 1.4 M⊙ neutron stars in a binary with separation of R⊙ observed from a distance of 1 kpc: ...
... An observer in the orbital plane has θ = π/2 and h× = 0. The observed frequency of gravitational waves is ν = Ω/π. The intensity of gravitational waves decreases as 1/r. Consider two 1.4 M⊙ neutron stars in a binary with separation of R⊙ observed from a distance of 1 kpc: ...
US - Real Science
... Around one quarter of all large stars are born in starburst galaxies such as this. They spawn stars up to a thousand times faster than the Milky Way. In most starbursts the surge in starbirth is triggered when two galaxies come too close together. Mutual attraction between the galaxies causes immens ...
... Around one quarter of all large stars are born in starburst galaxies such as this. They spawn stars up to a thousand times faster than the Milky Way. In most starbursts the surge in starbirth is triggered when two galaxies come too close together. Mutual attraction between the galaxies causes immens ...
CELESTIAL MANUAL:CELESTIAL MANUAL
... the point on the dials right ascension scale opposite 11.40 is in line with the point on the date scale corresponding to June 11. ...
... the point on the dials right ascension scale opposite 11.40 is in line with the point on the date scale corresponding to June 11. ...
Document
... • Equation of the degenerate electrons, • Although the temperature increases, the pressure and density do not change The core does not expand to cool. • The increase in the temperature leads a further increase in the rate of the release energy. ...
... • Equation of the degenerate electrons, • Although the temperature increases, the pressure and density do not change The core does not expand to cool. • The increase in the temperature leads a further increase in the rate of the release energy. ...
Galaxies (and stars) in the far infrared: results from the AKARI All
... photospheres of stars dominates the 9 μm catalogue: the galactic disc and nuclear bulge are clearly visible at this wavelength ...
... photospheres of stars dominates the 9 μm catalogue: the galactic disc and nuclear bulge are clearly visible at this wavelength ...
Put your title in here…
... Outline Structure Accretion Disruption Flare Wind Remnants Observation End ...
... Outline Structure Accretion Disruption Flare Wind Remnants Observation End ...
MODULE CODE: AHAN7024 TITLE: Heavenly Discourses DATED
... 8.3 The changing cultural perception of the sky: deep space and Hubble the current cultural view of the universe. 8.4 The re-emergences of naked-eye sky – the Dark Sky movement, WAN Night). ...
... 8.3 The changing cultural perception of the sky: deep space and Hubble the current cultural view of the universe. 8.4 The re-emergences of naked-eye sky – the Dark Sky movement, WAN Night). ...
X-ray binaries
... Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an accretion disc around a compact object. Clear classifiction is based on optical data or on mass function derived from X-ray observations. If a source is unidentified in optics, but exhibits T ...
... Also there are more and more LMXBs found in more distant galaxies. In optics the emission is dominated by an accretion disc around a compact object. Clear classifiction is based on optical data or on mass function derived from X-ray observations. If a source is unidentified in optics, but exhibits T ...
ppt - SLAC
... 1. Black-body temperature sets the star's color and determines its surface brightness: 2. Atmospheric pressure depends on the star's surface gravity and so, roughly, on its size —a giant, dwarf, or in between. The size and surface brightness yield the star's luminosity and often its evolutionary sta ...
... 1. Black-body temperature sets the star's color and determines its surface brightness: 2. Atmospheric pressure depends on the star's surface gravity and so, roughly, on its size —a giant, dwarf, or in between. The size and surface brightness yield the star's luminosity and often its evolutionary sta ...
Astronomy Assignment #1
... This question requires a fairly complete understanding of the celestial coordinate system and the celestial sphere model. According to the last sentence on page 43 “if a star’s declination matches your latitude it will pass over through zenith”. This means that the declination of your zenith is just ...
... This question requires a fairly complete understanding of the celestial coordinate system and the celestial sphere model. According to the last sentence on page 43 “if a star’s declination matches your latitude it will pass over through zenith”. This means that the declination of your zenith is just ...
The cosmic distance scale
... Thus if the star has a radius r0 at t0, and r1 at t1, the change in the bolometric apparent magnitude will be m1 – m0 = M1 – M0 = -2.5 log(L1/L0) = -5 log(r1/r0) - 10 log(T1/T0) Since r1 = r0 + ∆ r, if we measure T0 and T1, and ∆ r using the lineshifts in the spectrum, we can solve for r0, and ther ...
... Thus if the star has a radius r0 at t0, and r1 at t1, the change in the bolometric apparent magnitude will be m1 – m0 = M1 – M0 = -2.5 log(L1/L0) = -5 log(r1/r0) - 10 log(T1/T0) Since r1 = r0 + ∆ r, if we measure T0 and T1, and ∆ r using the lineshifts in the spectrum, we can solve for r0, and ther ...
White dwarf cooling sequences and cosmochronology
... Figure 3 displays the oxygen profiles for the CO core of a ∼ 0.6 M white dwarf progenitor obtained just at the end of the AGB phase (solid line). The inner part of the core, with a constant abundance of 16 O, is determined by the maximum extension of the central He-burning convective region while b ...
... Figure 3 displays the oxygen profiles for the CO core of a ∼ 0.6 M white dwarf progenitor obtained just at the end of the AGB phase (solid line). The inner part of the core, with a constant abundance of 16 O, is determined by the maximum extension of the central He-burning convective region while b ...
Recent science results from VLTI commissioning
... • Stellar parameters from lit (225km/s projected velocity etc) An extreme uniform Roche model with veq=vcrit and i=90° was also used Results: • Be star models don’t work • Extreme (equator-on, rotation at break-up speed) Roche model does but…it is not consistent with known properties of Be stars (no ...
... • Stellar parameters from lit (225km/s projected velocity etc) An extreme uniform Roche model with veq=vcrit and i=90° was also used Results: • Be star models don’t work • Extreme (equator-on, rotation at break-up speed) Roche model does but…it is not consistent with known properties of Be stars (no ...
VY Canis Majoris: The Astrophysical Basis of Its Luminosity
... photosphere or its surface directly. It has been known for some time that VY CMa’s absorption spectrum is significantly redshifted with respect to its systemic velocity (Humphreys 1975, Wallerstein 1977) due to scattering by dust (Herbig 1970, Kwok 1976, Van Blerkom & Van Blerkom 1978). Indeed, most ...
... photosphere or its surface directly. It has been known for some time that VY CMa’s absorption spectrum is significantly redshifted with respect to its systemic velocity (Humphreys 1975, Wallerstein 1977) due to scattering by dust (Herbig 1970, Kwok 1976, Van Blerkom & Van Blerkom 1978). Indeed, most ...
2 The Concept of “Spectral Classes”
... groups of like stars without making explicit searches by star name one at a time or by cross correlation of established catalogs. In fact, this is one of the most common requests the Multi-Mission Archive at the Space Telescope Science Institute (MAST) receives. The IUE satellite project, with the F ...
... groups of like stars without making explicit searches by star name one at a time or by cross correlation of established catalogs. In fact, this is one of the most common requests the Multi-Mission Archive at the Space Telescope Science Institute (MAST) receives. The IUE satellite project, with the F ...
16_Testbank
... 38) What prevents a brown dwarf from undergoing nuclear fusion? A) Degeneracy pressure halts the contraction of a protostar so the core never becomes hot or dense enough for nuclear fusion. B) There is not enough mass to maintain nuclear reactions in a self-sustaining way. C) The surface temperature ...
... 38) What prevents a brown dwarf from undergoing nuclear fusion? A) Degeneracy pressure halts the contraction of a protostar so the core never becomes hot or dense enough for nuclear fusion. B) There is not enough mass to maintain nuclear reactions in a self-sustaining way. C) The surface temperature ...
Ursa Minor
Ursa Minor (Latin: ""Smaller She-Bear"", contrasting with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the name Little Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, due to Polaris being the North Star.Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from apparent magnitude 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and magnitude 3 Gamma Ursae Minoris have been called the ""guardians of the pole star"". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered with a surface temperature of 200,000 K.