Spiral Arms - Harry Kroto
... them wrap into a spiral due to the fact that the inner parts will revolve around the Galactic center faster than the outer parts. We can see that a nice spiral forms very quickly. The problem is that the spiral continues wind up tighter and tigher. In only a few revolutions the spiral gets extremely ...
... them wrap into a spiral due to the fact that the inner parts will revolve around the Galactic center faster than the outer parts. We can see that a nice spiral forms very quickly. The problem is that the spiral continues wind up tighter and tigher. In only a few revolutions the spiral gets extremely ...
teach with space
... For any system in space where two or more objects are orbiting each other, the system will have a centre of mass, or barycentre, about which all bodies orbit. The simple case: a two-body system For the simple case of a two-body system, the centre of mass or barycentre is the point around which both ...
... For any system in space where two or more objects are orbiting each other, the system will have a centre of mass, or barycentre, about which all bodies orbit. The simple case: a two-body system For the simple case of a two-body system, the centre of mass or barycentre is the point around which both ...
• Teacher developed presentations. • Teacher developed laboratory
... What are the different classifications of galaxies? How can we distinguish between planets and other objects in the solar system based on characteristics? What are the different phases of the moon? How are the location and properties of exoplanets identified? How is the constancy of the speed of lig ...
... What are the different classifications of galaxies? How can we distinguish between planets and other objects in the solar system based on characteristics? What are the different phases of the moon? How are the location and properties of exoplanets identified? How is the constancy of the speed of lig ...
Paper - AMOS Conference
... optical system and texp is the exposure time, and in most of the cases we examine, the object making the streak is in the field of view both at the beginning and end of the exposure so these are the same. Rstreak is the rate of growth of the streak in pixels per second – if the streak is undersample ...
... optical system and texp is the exposure time, and in most of the cases we examine, the object making the streak is in the field of view both at the beginning and end of the exposure so these are the same. Rstreak is the rate of growth of the streak in pixels per second – if the streak is undersample ...
Project Description - SDSS-III
... Universe imprint a characteristic scale on the clustering of dark matter, galaxies, and intergalactic gas. By measuring this scale with tracers seen at different redshifts, we can create a “Hubble diagram” of unprecedented precision covering most of cosmic history and can thereby pin down the prope ...
... Universe imprint a characteristic scale on the clustering of dark matter, galaxies, and intergalactic gas. By measuring this scale with tracers seen at different redshifts, we can create a “Hubble diagram” of unprecedented precision covering most of cosmic history and can thereby pin down the prope ...
1 - Piscataway High School
... of the gas would weigh more than an automobile. In this degenerate matter, the pressure does not depend on temperature, and that means the pressure–temperature thermostat does not regulate energy production. When the temperature becomes hot enough, helium fusion begins to make energy, and the temper ...
... of the gas would weigh more than an automobile. In this degenerate matter, the pressure does not depend on temperature, and that means the pressure–temperature thermostat does not regulate energy production. When the temperature becomes hot enough, helium fusion begins to make energy, and the temper ...
Stellar Spectroscopy
... measure of the quantity of each color of light (or more specifically, the amount of each wavelength of light). It is a powerful tool in astronomy. In fact, most of what we know in astronomy is a result of spectroscopy: it can reveal the temperature, velocity and composition of an object as well as b ...
... measure of the quantity of each color of light (or more specifically, the amount of each wavelength of light). It is a powerful tool in astronomy. In fact, most of what we know in astronomy is a result of spectroscopy: it can reveal the temperature, velocity and composition of an object as well as b ...
Planetary Nebulae: Observational Properties, Mimics, and Diagnostics
... As befits the large range in apparent size, morphology, integrated flux, surface brightness, excitation class, central star magnitude, and evolutionary state shown by individual PN, a large and diverse range of detection methods has been used in their discovery. Some of the brightest and best-known ...
... As befits the large range in apparent size, morphology, integrated flux, surface brightness, excitation class, central star magnitude, and evolutionary state shown by individual PN, a large and diverse range of detection methods has been used in their discovery. Some of the brightest and best-known ...
P1 topic 3 - WordPress.com
... (iii) One theory of the origin of the Universe predicted that there should be cosmic background radiation with a wavelength of about 1 mm. Explain why scientists had to wait until the development of space flight before they could study this radiation in detail. ...
... (iii) One theory of the origin of the Universe predicted that there should be cosmic background radiation with a wavelength of about 1 mm. Explain why scientists had to wait until the development of space flight before they could study this radiation in detail. ...
Comparing stars - The Open University
... than the Sun, and appears bluish-white. It has the greatest apparent visual brightness (most negative apparent visual magnitude!) of any star in the night sky. This is, as we have seen, not because it is very luminous, but because it is both fairly luminous and rather close - at 2.63 pc it's the sev ...
... than the Sun, and appears bluish-white. It has the greatest apparent visual brightness (most negative apparent visual magnitude!) of any star in the night sky. This is, as we have seen, not because it is very luminous, but because it is both fairly luminous and rather close - at 2.63 pc it's the sev ...
The Kuiper Belt Explored by Serendipitous Stellar Occultations
... R* is the radius of the star projected at the distance of the occulting object. Note that if the star’s apparent size is known, the occultation profile provides some information on the object’s size without any hypothesis about its albedo. The angular sizes of the stars depend on their spectral and ...
... R* is the radius of the star projected at the distance of the occulting object. Note that if the star’s apparent size is known, the occultation profile provides some information on the object’s size without any hypothesis about its albedo. The angular sizes of the stars depend on their spectral and ...
Lecture26_Future
... The Unique Universe: There is a deep underlying principle of physics that requires the universe to be this way. Some “Theory of Everything” will explain why the various features of the Universe must have exactly the values that we see. We just haven’t found it yet. ...
... The Unique Universe: There is a deep underlying principle of physics that requires the universe to be this way. Some “Theory of Everything” will explain why the various features of the Universe must have exactly the values that we see. We just haven’t found it yet. ...
Wide-field CCD imager for the 6.5m MMT telescope
... Autoguiding will be done with two additional 2kx4k (possibly unthinned or otherwise not quite perfect) CCDs in the focal plane. These devices will be operated in frame-transfer mode, giving an active area of 2kx2k pixels. Stars can be located by reading out the full array. Subsequently, a small area ...
... Autoguiding will be done with two additional 2kx4k (possibly unthinned or otherwise not quite perfect) CCDs in the focal plane. These devices will be operated in frame-transfer mode, giving an active area of 2kx2k pixels. Stars can be located by reading out the full array. Subsequently, a small area ...
Mapping the Milky Way: William Herschel`s Star-‐Gages
... What about violations of assumption 1 above? To let users explore this scenario, Herschel’s Star Gages includes virtual star systems with non-‐uniform distributions of stars. Figure 6 illustrates one su ...
... What about violations of assumption 1 above? To let users explore this scenario, Herschel’s Star Gages includes virtual star systems with non-‐uniform distributions of stars. Figure 6 illustrates one su ...
Star formation and internal kinematics of irregular galaxies
... (a few times) the local scale height. In most cases this is a few hundred parsecs. This is the picture that I will proceed with in this thesis; that star formation is a local process, with the same basic physics occuring in independent cells with dimensions between tens of parsecs and a couple of ki ...
... (a few times) the local scale height. In most cases this is a few hundred parsecs. This is the picture that I will proceed with in this thesis; that star formation is a local process, with the same basic physics occuring in independent cells with dimensions between tens of parsecs and a couple of ki ...
Geometry of orbits - Harpursville Middle School
... shorter wavelength blue end of the spectrum or to the longer wavelength red end of the spectrum ...
... shorter wavelength blue end of the spectrum or to the longer wavelength red end of the spectrum ...
THE ABSOLUTE MAGNITUDE OF RR LYRAE - Cosmos
... The absolute magnitude (MV ) of RR Lyrae stars is an indicator for distance and age in our Galaxy. Especially it is a key parameter to determine the age of Galactic globular clusters. However, the value of MV de es a consensus and splits into a faint value and a bright value. The faint value of MV ...
... The absolute magnitude (MV ) of RR Lyrae stars is an indicator for distance and age in our Galaxy. Especially it is a key parameter to determine the age of Galactic globular clusters. However, the value of MV de es a consensus and splits into a faint value and a bright value. The faint value of MV ...
Distance determination for RAVE stars using stellar models
... used to illuminate a host of substructures in the Galactic halo. The strength of photometric distances is that they can be constructed for a wide range of stellar populations. An important recent study was carried out by Ivezić et al. (2008). In this work they took high-precision multi-band optical ...
... used to illuminate a host of substructures in the Galactic halo. The strength of photometric distances is that they can be constructed for a wide range of stellar populations. An important recent study was carried out by Ivezić et al. (2008). In this work they took high-precision multi-band optical ...
AST1100 Lecture Notes
... core, the star originally had more mass which was blown off) the radius of the white dwarf is similar to the radius of the Earth. A white dwarf is thus extremely dense, one solar mass compressed roughly to the size of the Earth. There is another interesting relation to be extracted from this equatio ...
... core, the star originally had more mass which was blown off) the radius of the white dwarf is similar to the radius of the Earth. A white dwarf is thus extremely dense, one solar mass compressed roughly to the size of the Earth. There is another interesting relation to be extracted from this equatio ...