Astro-MilkyWay
... 5. What fundamental principle did Shapley use to calibrate the period-luminosity relationship for Cepheid variable stars? a. Light intensity falls off with the inverse square of distance. b. Stars that appear brighter are on average closer to Earth. c. Large pulsating objects have longer periods tha ...
... 5. What fundamental principle did Shapley use to calibrate the period-luminosity relationship for Cepheid variable stars? a. Light intensity falls off with the inverse square of distance. b. Stars that appear brighter are on average closer to Earth. c. Large pulsating objects have longer periods tha ...
Society News - Bristol Astronomical Society
... As we move into the autumn season, the longer nights become more noticeable, allowing observing to take place at a more sociable time. This month, low in the southern sky you will find a faint group of constellations which are collectively known as ‘The Water’. The members of this group are Cetus, C ...
... As we move into the autumn season, the longer nights become more noticeable, allowing observing to take place at a more sociable time. This month, low in the southern sky you will find a faint group of constellations which are collectively known as ‘The Water’. The members of this group are Cetus, C ...
The Milky Way
... 5. What fundamental principle did Shapley use to calibrate the period-luminosity relationship for Cepheid variable stars? a. Light intensity falls off with the inverse square of distance. b. Stars that appear brighter are on average closer to Earth. c. Large pulsating objects have longer periods tha ...
... 5. What fundamental principle did Shapley use to calibrate the period-luminosity relationship for Cepheid variable stars? a. Light intensity falls off with the inverse square of distance. b. Stars that appear brighter are on average closer to Earth. c. Large pulsating objects have longer periods tha ...
Planets and Moons - Fraser Heights Chess Club
... • A galaxy is an enormous collection of gas, dust and billions of stars held together by gravity. One galaxy can have hundreds of billions of stars and be as large as 200,000 light years across. • Galaxy is derived from the Greek galaxias meaning "milky", a reference to the Milky Way. • Many galaxie ...
... • A galaxy is an enormous collection of gas, dust and billions of stars held together by gravity. One galaxy can have hundreds of billions of stars and be as large as 200,000 light years across. • Galaxy is derived from the Greek galaxias meaning "milky", a reference to the Milky Way. • Many galaxie ...
Issue 118 - Apr 2014
... How to Get Started with Variable Star Observing Adapted from Astronomical League article by Robert Togni [Editor's Note: The May 13 public meeting at the Florida Museum features Dr. Mario Motto as our guest speaker. A former president of the American Association of Variable Star Observers, Dr. Motto ...
... How to Get Started with Variable Star Observing Adapted from Astronomical League article by Robert Togni [Editor's Note: The May 13 public meeting at the Florida Museum features Dr. Mario Motto as our guest speaker. A former president of the American Association of Variable Star Observers, Dr. Motto ...
1.2.43The stellar populations of the Milky Way
... Pop. II stars occupy the spheroid – the stellar halo and bulge – and turn out to be the oldest stars known, with ages in the range (12 to 15) × 1091yr. Conspicuous examples are globular-cluster stars. Little or no interstellar gas is still associated with Pop. II stars, which is consistent with star ...
... Pop. II stars occupy the spheroid – the stellar halo and bulge – and turn out to be the oldest stars known, with ages in the range (12 to 15) × 1091yr. Conspicuous examples are globular-cluster stars. Little or no interstellar gas is still associated with Pop. II stars, which is consistent with star ...
The correct answers are written in bold, italic and underlined. The
... The most massive stars are the most luminous, while less massive stars are distributed down the ZAMS. 2. On the main sequence of the Hertsprung-Russell diagram of a very young cluster, where will the most massive stars be found? • At the very bottom of the main sequence, massive stars being cool bec ...
... The most massive stars are the most luminous, while less massive stars are distributed down the ZAMS. 2. On the main sequence of the Hertsprung-Russell diagram of a very young cluster, where will the most massive stars be found? • At the very bottom of the main sequence, massive stars being cool bec ...
Siriusposter
... white dwarfs. At these energies, white dwarfs are far brighter than most normal stars, and with ROSAT’s help we have been able to identify over 20 of these degenerate objects in binaries with bright, normal companions, just like the Sirius system. At optical wavelengths the white dwarfs are unresolv ...
... white dwarfs. At these energies, white dwarfs are far brighter than most normal stars, and with ROSAT’s help we have been able to identify over 20 of these degenerate objects in binaries with bright, normal companions, just like the Sirius system. At optical wavelengths the white dwarfs are unresolv ...
Galaxies
... are also nearly all the same color: somewhat redder than the Sun. On the tuning fork diagram, they are classified as E, followed by a number indicating how elliptical a given galaxy is. The higher the number, the more elliptical the galaxy; that is, the longer the galaxy is with respect to its width ...
... are also nearly all the same color: somewhat redder than the Sun. On the tuning fork diagram, they are classified as E, followed by a number indicating how elliptical a given galaxy is. The higher the number, the more elliptical the galaxy; that is, the longer the galaxy is with respect to its width ...
Unlocking galaxy formation histories with SAMI
... › The spectra: - Large spectral range covering many prominent absorption features - Intermediate resolution suitable for most galaxies – allows us to separate emission and absorption ...
... › The spectra: - Large spectral range covering many prominent absorption features - Intermediate resolution suitable for most galaxies – allows us to separate emission and absorption ...
The ISM and Stellar Birth
... • Near the Sun, Extinction amounts to 2 magnitudes per 1000 parsecs. That is, a star 1000pc from Earth will look about 2 magnitudes fainter than if space were empty completely • Dust thought to come from stellar ‘winds’, blowing out molecules of hydrogen, carbon, oxygen and other elements which coo ...
... • Near the Sun, Extinction amounts to 2 magnitudes per 1000 parsecs. That is, a star 1000pc from Earth will look about 2 magnitudes fainter than if space were empty completely • Dust thought to come from stellar ‘winds’, blowing out molecules of hydrogen, carbon, oxygen and other elements which coo ...
Activity Book Level 4
... appears like a band because it is a disc-shaped structure being viewed from inside. That this faint band of light is made up of stars was proven in 1610 when Galileo Galilei used his telescope to resolve it into individual stars. In the 1920s, observations by astronomer Edwin Hubble showed that the ...
... appears like a band because it is a disc-shaped structure being viewed from inside. That this faint band of light is made up of stars was proven in 1610 when Galileo Galilei used his telescope to resolve it into individual stars. In the 1920s, observations by astronomer Edwin Hubble showed that the ...
Stars and Galaxies - La Salle Elementary Public Schools No 122
... Life Cycle of a Star (cont.) • When a star’s hydrogen supply is nearly gone, the star leaves the main sequence and begins the next stage of its life cycle. • All stars form in the same way, but stars die in different ways, depending on their masses. • Massive stars eventually become red ...
... Life Cycle of a Star (cont.) • When a star’s hydrogen supply is nearly gone, the star leaves the main sequence and begins the next stage of its life cycle. • All stars form in the same way, but stars die in different ways, depending on their masses. • Massive stars eventually become red ...
The galaxy correlation function and power spec- trum
... where n is the mean density of galaxies (which is the same in real space and redshift space, even though the clustering properties vary between the two.) ...
... where n is the mean density of galaxies (which is the same in real space and redshift space, even though the clustering properties vary between the two.) ...
hubble_refurb
... supersonic shock wave in the surrounding medium and making the material glow. The Hubble visible-light image reveals, deep within the remnant, a crescent-shaped cloud of pink emission from hydrogen gas and soft purple wisps that correspond to regions of glowing oxygen. A dense background of colorful ...
... supersonic shock wave in the surrounding medium and making the material glow. The Hubble visible-light image reveals, deep within the remnant, a crescent-shaped cloud of pink emission from hydrogen gas and soft purple wisps that correspond to regions of glowing oxygen. A dense background of colorful ...
the summary
... A GRB afterglow can be observed over a broad range of wavelengths: from X-rays, ultraviolet to optical, infrared and radio waves. All of this radiation is light; only the energy per photon (or equivalently wavelength, or frequency) is different. While the initial gamma-rays are observed from space w ...
... A GRB afterglow can be observed over a broad range of wavelengths: from X-rays, ultraviolet to optical, infrared and radio waves. All of this radiation is light; only the energy per photon (or equivalently wavelength, or frequency) is different. While the initial gamma-rays are observed from space w ...
here in Powerpoint format
... bA is the apparent brightness of star A bB is the apparent brightness of star B mA is the apparent magnitude of star A mB is the apparent magnitude of star B ...
... bA is the apparent brightness of star A bB is the apparent brightness of star B mA is the apparent magnitude of star A mB is the apparent magnitude of star B ...
Tasks - ESA Science
... The magnification method takes the 1994 image and magnifies it until it exactly matches the 1997 image. Fig. 7 shows the method of subtracting. Note that the image taken in 1994 is not magnified. In each of the nine small images in Fig. 8 the 1994 image was magnified by a different factor, F, (this ...
... The magnification method takes the 1994 image and magnifies it until it exactly matches the 1997 image. Fig. 7 shows the method of subtracting. Note that the image taken in 1994 is not magnified. In each of the nine small images in Fig. 8 the 1994 image was magnified by a different factor, F, (this ...
English - Wise Observatory
... makes up 23% of the Universe while the luminous matter is only a few percent. Although the nature of the dark matter is sill unknown, theoretical simulations indicated that the Universe is peppered by dark matter concentrations called “dark halos”. These halos attract intergalactic gas that turns in ...
... makes up 23% of the Universe while the luminous matter is only a few percent. Although the nature of the dark matter is sill unknown, theoretical simulations indicated that the Universe is peppered by dark matter concentrations called “dark halos”. These halos attract intergalactic gas that turns in ...
Astrometry of Binary Stars: What Are We Waiting For?
... An exquisite orbit! dP/P = 0.00041 da/a = 0.00137 Hipparcos distance ~30 pc dp/p = 0.02628 Gaia: dp/p ~ 0.0006. Then you’ll get great masses! ...
... An exquisite orbit! dP/P = 0.00041 da/a = 0.00137 Hipparcos distance ~30 pc dp/p = 0.02628 Gaia: dp/p ~ 0.0006. Then you’ll get great masses! ...
Milky Way Galaxy
... The Universe is filled with these star systems which themselves cluster together into larger systems. ...
... The Universe is filled with these star systems which themselves cluster together into larger systems. ...
the galaxy in which we live - Cosmos
... information for stars in a reduced area of the Galaxy, around the Sun (see drawing). This has been achieved with the data gathered by the Hipparcos satellite, launched by ESA in 1989. But clearly, conclusions about the large-scale structure and dynamics of our Milky Way need a much deeper and more e ...
... information for stars in a reduced area of the Galaxy, around the Sun (see drawing). This has been achieved with the data gathered by the Hipparcos satellite, launched by ESA in 1989. But clearly, conclusions about the large-scale structure and dynamics of our Milky Way need a much deeper and more e ...
Week 10
... On Earth, the parallax angle measured for the star Procyon is 0.29 arcseconds. If you were to measure Procyon’s parallax angle from Venus, what would the parallax angle be? (Note: Venus’ orbit is smaller than Earth’s orbit.) A. More than 0.29 arcseconds B. 0.29 arcseconds C. Less than 0.29 arcsecond ...
... On Earth, the parallax angle measured for the star Procyon is 0.29 arcseconds. If you were to measure Procyon’s parallax angle from Venus, what would the parallax angle be? (Note: Venus’ orbit is smaller than Earth’s orbit.) A. More than 0.29 arcseconds B. 0.29 arcseconds C. Less than 0.29 arcsecond ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.