Spring Constellations
... Virgo, the virgin. Her head is right under Leo’s tail & she’s reclining on a couch. Only bright star is Spica which means “ear of wheat.” Spica is a white star (hot), about 220 LY away, & 2000X the sun’s brightness. A whole group of galaxies is to the left of Leo’s tail & above Virgo’s head. The Som ...
... Virgo, the virgin. Her head is right under Leo’s tail & she’s reclining on a couch. Only bright star is Spica which means “ear of wheat.” Spica is a white star (hot), about 220 LY away, & 2000X the sun’s brightness. A whole group of galaxies is to the left of Leo’s tail & above Virgo’s head. The Som ...
THE GALACTIC GAZETTE The Astronomical Society of Southern New England Next Meeting
... Globular clusters are too cool. For one thing, they’re gorgeous. I have proof! That is IC 4499, a tight ball of tens or hundreds of thousands of stars located roughly 60,000 light years away. This image was taken by Hubble, and besides being spectacular, it also was used to nail down the age of the ...
... Globular clusters are too cool. For one thing, they’re gorgeous. I have proof! That is IC 4499, a tight ball of tens or hundreds of thousands of stars located roughly 60,000 light years away. This image was taken by Hubble, and besides being spectacular, it also was used to nail down the age of the ...
PC3692: Physics of Stellar Structure (and Evolution)
... Therefore, we have So the radius of a star, the effective temperature and luminosity are related, and if we can measure two of them, then we can determine the remaining third parameter. Fig. 4 illustrates the spectrum of the Sun. The top panel shows a low-resolution spectrum while the right panel sh ...
... Therefore, we have So the radius of a star, the effective temperature and luminosity are related, and if we can measure two of them, then we can determine the remaining third parameter. Fig. 4 illustrates the spectrum of the Sun. The top panel shows a low-resolution spectrum while the right panel sh ...
*Studying Complex Star-Forming Fields: Rosette Nebula and Monoceros Loop by Chris Hathaway and Anthony Kuchera
... difficult one to obtain. The direct method to find stellar distances is the method of stellar parallax, based on the revolution of the Earth around the Sun. Unfortunately, from the surface of the Earth, parallaxes of stars located even in the nearest star-forming fields cannot be obtained—the stars ...
... difficult one to obtain. The direct method to find stellar distances is the method of stellar parallax, based on the revolution of the Earth around the Sun. Unfortunately, from the surface of the Earth, parallaxes of stars located even in the nearest star-forming fields cannot be obtained—the stars ...
Stellar Spectroscopy (GA 3.0) - National Optical Astronomy
... some stars, emission lines as well. These spectral lines can be used to determine an incredible amount of information about the star, including its temperature, composition, size, velocity and age, as well as many other properties. Most of what we know about stars has been determined by the study of ...
... some stars, emission lines as well. These spectral lines can be used to determine an incredible amount of information about the star, including its temperature, composition, size, velocity and age, as well as many other properties. Most of what we know about stars has been determined by the study of ...
PSF - ESO
... First you must FIND the stellar-appearing objects in the frame. Each program has its own method - sometimes several methods – of performing this, but the basic idea is to produce an initial list of approximate centroid positions for all stars that can be distinguished in the two dimensional data arr ...
... First you must FIND the stellar-appearing objects in the frame. Each program has its own method - sometimes several methods – of performing this, but the basic idea is to produce an initial list of approximate centroid positions for all stars that can be distinguished in the two dimensional data arr ...
lect3 — 1 Measuring stars: What can be measured?
... apparent position of the object over a 6-month baseline (θ). The earth moves 2 AU, so then tanθ = 1A.U./D ≈ θ (using the small-angle approximation). An angle of 1 arcsecond then corresponds to D ≡ 3.086 × 1018 cm. This is known as a parsec (PARallax arcSECond). Unfortunately, this only works for qui ...
... apparent position of the object over a 6-month baseline (θ). The earth moves 2 AU, so then tanθ = 1A.U./D ≈ θ (using the small-angle approximation). An angle of 1 arcsecond then corresponds to D ≡ 3.086 × 1018 cm. This is known as a parsec (PARallax arcSECond). Unfortunately, this only works for qui ...
Stellar Evolution in the HR Diagram
... Electron degeneracy cannot support cores more massive than 1.4 M. If a degenerate C/O core (i.e., a white dwarf) is pushed above this limit, it was collapse and begin fusing, but it will not have time to adjust its structure (all the energy will just go into lifting the degeneracy). The star will b ...
... Electron degeneracy cannot support cores more massive than 1.4 M. If a degenerate C/O core (i.e., a white dwarf) is pushed above this limit, it was collapse and begin fusing, but it will not have time to adjust its structure (all the energy will just go into lifting the degeneracy). The star will b ...
Exam #2 Solutions
... The cooler giant stars are mostly K and M giants with temperatures around 5,000 K to 3,000K and luminosities between 50 and 5,000 solar luminosities. The stars are all larger in radius than the Sun, being between 1 and 100 solar radii. All these stars will have very short lifetimes compared to ...
... The cooler giant stars are mostly K and M giants with temperatures around 5,000 K to 3,000K and luminosities between 50 and 5,000 solar luminosities. The stars are all larger in radius than the Sun, being between 1 and 100 solar radii. All these stars will have very short lifetimes compared to ...
Read the information on Hertzsprung
... radiates in one second, but you can think of it as how bright or how dim the star appears. The luminosity scale is a "ratio scale" in which stars are compared to each other based upon a reference (our sun). The horizontal axis represents the star’s surface temperature (not the star’s core temperatur ...
... radiates in one second, but you can think of it as how bright or how dim the star appears. The luminosity scale is a "ratio scale" in which stars are compared to each other based upon a reference (our sun). The horizontal axis represents the star’s surface temperature (not the star’s core temperatur ...
Astrophysics notes
... methods for photometry (8 marks) Not restricted to visible spectrum, much wider range of Use a high resolution charge-coupled device (CCD) so pictures are good, although photographic can sometimes get even higher resolution. It is an electronic signal, so it can be MULTIPLIED DIGITISED ANAL ...
... methods for photometry (8 marks) Not restricted to visible spectrum, much wider range of Use a high resolution charge-coupled device (CCD) so pictures are good, although photographic can sometimes get even higher resolution. It is an electronic signal, so it can be MULTIPLIED DIGITISED ANAL ...
Evolution of Warm Debris Around Sun-like Stars: Clues to Terrestrial
... non-linear least squares fit for temperature, solid angle (radius/distance), and extinction. For stars within 50 pc, we assumed Av=0. Photometry at 24 microns was derived from observations with the MIPS instrument (Rieke et al. 2004). We began with SSC pipeline data (version 14.2) and photometry wa ...
... non-linear least squares fit for temperature, solid angle (radius/distance), and extinction. For stars within 50 pc, we assumed Av=0. Photometry at 24 microns was derived from observations with the MIPS instrument (Rieke et al. 2004). We began with SSC pipeline data (version 14.2) and photometry wa ...
Magnitude Scale and Distance Measurements
... Distance formula: r = 10 You will need to apply this later on, when we determine the distance to a star cluster by curve-fitting on the H-R Diagram. 1) The absolute magnitude of the Sun is +4.83, of Sirius A is + 1.45, and of Spica is .119. Using the apparent magnitudes given in part 1 of this revie ...
... Distance formula: r = 10 You will need to apply this later on, when we determine the distance to a star cluster by curve-fitting on the H-R Diagram. 1) The absolute magnitude of the Sun is +4.83, of Sirius A is + 1.45, and of Spica is .119. Using the apparent magnitudes given in part 1 of this revie ...
Glossary Topics - Home - DMNS Galaxy Guide Portal
... layers. Such stars also become blue and red supergiants. As they build up an iron core, they too explode as supernovae. The remaining core then begins to collapse. If the core is larger than five solar masses, collapse continues until it becomes a black hole. If the core is less than five solar mass ...
... layers. Such stars also become blue and red supergiants. As they build up an iron core, they too explode as supernovae. The remaining core then begins to collapse. If the core is larger than five solar masses, collapse continues until it becomes a black hole. If the core is less than five solar mass ...
Visual Double Star Measurements with Equatorial - Alt
... the telescope and does not require repetitive two star alignments. The eyepiece is then rotated until the double stars are aligned on the linear scale. Then the telescope is moved so that the primary star accurately drifts through the central division mark. In practice, the primary is situated about ...
... the telescope and does not require repetitive two star alignments. The eyepiece is then rotated until the double stars are aligned on the linear scale. Then the telescope is moved so that the primary star accurately drifts through the central division mark. In practice, the primary is situated about ...
UCAC4 is a compiled, all-sky star catalog covering mainly the 8 to
... UCAC4 is a compiled, all-sky star catalog covering mainly the 8 to 16 magnitude range in a single bandpass between V and R. Positional errors are about 15 to 20 mas for stars in the 10 to 14 mag range. Proper motions have been derived for most of the about 113 million stars utilizing about 140 other ...
... UCAC4 is a compiled, all-sky star catalog covering mainly the 8 to 16 magnitude range in a single bandpass between V and R. Positional errors are about 15 to 20 mas for stars in the 10 to 14 mag range. Proper motions have been derived for most of the about 113 million stars utilizing about 140 other ...
Module code: AA1
... reason their below average luminosity is sufficient to make them appear on the list of the 20 brightest stars. The sample group of the nearest stars is more representative than the group of the brightest stars when wanting to make a statement about the main type of stars in our galaxy as they do not ...
... reason their below average luminosity is sufficient to make them appear on the list of the 20 brightest stars. The sample group of the nearest stars is more representative than the group of the brightest stars when wanting to make a statement about the main type of stars in our galaxy as they do not ...
26.4 Groups of Stars
... Star Systems Sometimes the smaller star in a binary star is too dim to be seen easily from Earth but can still be detected from the motion of the other star. If one star passes in front of the other, blocking some of the light from reaching Earth, the star system is called an eclipsing binary. The b ...
... Star Systems Sometimes the smaller star in a binary star is too dim to be seen easily from Earth but can still be detected from the motion of the other star. If one star passes in front of the other, blocking some of the light from reaching Earth, the star system is called an eclipsing binary. The b ...
01-Star Atlas Project - Mapping the Heavens
... brightest star in the constellation of Lyra is α Lyrae, the second Figure 1-2 brightest star in Lyra is β Lyrae, and so on. Unfortunately, most constellations have more stars than there are Greek letters. So when Bayer ran out of Greek letters, he switched to lower case Roman letters (a,b,c ...). Wh ...
... brightest star in the constellation of Lyra is α Lyrae, the second Figure 1-2 brightest star in Lyra is β Lyrae, and so on. Unfortunately, most constellations have more stars than there are Greek letters. So when Bayer ran out of Greek letters, he switched to lower case Roman letters (a,b,c ...). Wh ...
Project 2. CCD Photometry
... 5. Standard stars and transformation equations Standard stars are required so that different observers are able to compare results with each other. The reason this is true is because every observational setup is likely to have different response functions, so the same stars will not be observed t ...
... 5. Standard stars and transformation equations Standard stars are required so that different observers are able to compare results with each other. The reason this is true is because every observational setup is likely to have different response functions, so the same stars will not be observed t ...
Magnitude of Stars - What`s Out Tonight?
... Although this movement may seem like it would be unnoticable, it was known by the ancient Egyptians because they took accurate measurements of where stars rose and set over hundreds and thousands of years. The effect of precession is that the Earth’s north pole points to different directions in the ...
... Although this movement may seem like it would be unnoticable, it was known by the ancient Egyptians because they took accurate measurements of where stars rose and set over hundreds and thousands of years. The effect of precession is that the Earth’s north pole points to different directions in the ...
AST 112 – Activity #4 The Stellar Magnitude System
... To calculate using base-ten logarithms To set the scale for apparent magnitudes To define absolute magnitude in terms of apparent magnitude and distance To determine the distance to a star given its apparent and absolute magnitudes ...
... To calculate using base-ten logarithms To set the scale for apparent magnitudes To define absolute magnitude in terms of apparent magnitude and distance To determine the distance to a star given its apparent and absolute magnitudes ...
Lec2015_22
... Initial Survey to Identify Potential Candidates • Need low-resolution spectra, or, now, with high accuracyphotometry, to identify stars that show low absorption below 4000 Angstroms • Historically, until last five years, “objective-prism” spectra employed • New wide-field photometric surveys allow ...
... Initial Survey to Identify Potential Candidates • Need low-resolution spectra, or, now, with high accuracyphotometry, to identify stars that show low absorption below 4000 Angstroms • Historically, until last five years, “objective-prism” spectra employed • New wide-field photometric surveys allow ...
Stars in Motion
... by the other. The thin, light colored band running down the horizontal centerline of the image is the absorption spectrum of the (spectral type A) star being observed. Dark vertical lines in this band represent absorption in the star, and are the lines that are of interest for calculating Doppler sh ...
... by the other. The thin, light colored band running down the horizontal centerline of the image is the absorption spectrum of the (spectral type A) star being observed. Dark vertical lines in this band represent absorption in the star, and are the lines that are of interest for calculating Doppler sh ...
PowerPoint - Louisiana State University
... Contemporary with Roman sculptor From Ptolemy’s Almagest From Aratus’ Phaenomena From Eudoxus’ Phaenomena Assyrian observer who was source for Eudoxus and MUL.APIN ...
... Contemporary with Roman sculptor From Ptolemy’s Almagest From Aratus’ Phaenomena From Eudoxus’ Phaenomena Assyrian observer who was source for Eudoxus and MUL.APIN ...
Star catalogue
A star catalogue, or star catalog, is an astronomical catalogue that lists stars. In astronomy, many stars are referred to simply by catalogue numbers. There are a great many different star catalogues which have been produced for different purposes over the years, and this article covers only some of the more frequently quoted ones. Star catalogues were compiled by many different ancient peoples, including the Babylonians, Greeks, Chinese, Persians, and Arabs. Most modern catalogues are available in electronic format and can be freely downloaded from NASA's Astronomical Data Center.Completeness and accuracy is described by the weakest apparent magnitude V (largest number) and the accuracy of the positions.