Calculating Parallax Lab
... Even when observed with the largest telescopes, stars are still just points of light. Although we may be able to tell a lot about a star through its light, these observations do not give us a reference scale to use to measure their distances. We need to rely on a method that you are actually already ...
... Even when observed with the largest telescopes, stars are still just points of light. Although we may be able to tell a lot about a star through its light, these observations do not give us a reference scale to use to measure their distances. We need to rely on a method that you are actually already ...
The Magnitude Scale
... where Fν is the flux per unit frequency received from the source, and F ν0 is a normalising constant. The normalising constants have been calibrated for standard photometric bands, some of which are listed in table 1 below. Notice that a larger value of the magnitude means that the source is fainter ...
... where Fν is the flux per unit frequency received from the source, and F ν0 is a normalising constant. The normalising constants have been calibrated for standard photometric bands, some of which are listed in table 1 below. Notice that a larger value of the magnitude means that the source is fainter ...
PARALLAX – IT`S SIMPLE! Abstract
... needed to calculate the real energy output of the star (luminosity). Other physical properties (core temperature, radius, mass) are also connected to the star’s luminosity. How far can parallax measurements reach? The diameter of our Galaxy is about 30 thousands parsecs, so it is clear that the HIPP ...
... needed to calculate the real energy output of the star (luminosity). Other physical properties (core temperature, radius, mass) are also connected to the star’s luminosity. How far can parallax measurements reach? The diameter of our Galaxy is about 30 thousands parsecs, so it is clear that the HIPP ...
File
... around another axis due to a torque (such as gravitational influence) acting to change the direction of the first axis – it means that we will have a new north star about 12,000 years from now 13. What are the 7 types of satellites and how is each used? Scientific research - Gather data for scientif ...
... around another axis due to a torque (such as gravitational influence) acting to change the direction of the first axis – it means that we will have a new north star about 12,000 years from now 13. What are the 7 types of satellites and how is each used? Scientific research - Gather data for scientif ...
300 MHz - 3 GHz Yes, we`re interested
... • Diffuse HI (cosmic web) - IGM-galaxy feedback poorly understood aspect of galaxy formation • Local HI mass function, probe low-mass end, in various environments HVC/dwarfs ...
... • Diffuse HI (cosmic web) - IGM-galaxy feedback poorly understood aspect of galaxy formation • Local HI mass function, probe low-mass end, in various environments HVC/dwarfs ...
Study Guide Ch10,11 and 12
... to explain their energy output and other characteristics. 11. Briefly relate the story of the discovery of quasars 12. Describe the current explanation of quasars and their energy sources. ...
... to explain their energy output and other characteristics. 11. Briefly relate the story of the discovery of quasars 12. Describe the current explanation of quasars and their energy sources. ...
docx - STAO
... The effects of temperature and brightness may be discussed. Betelgeuse is 15 times bigger (in radius) than Rigel and it is closer by more than 100 ly. Why is Rigel brighter? The explanation is that Betelgeuse is a red supergiant star that has evolved off the main sequence. This means that it has bur ...
... The effects of temperature and brightness may be discussed. Betelgeuse is 15 times bigger (in radius) than Rigel and it is closer by more than 100 ly. Why is Rigel brighter? The explanation is that Betelgeuse is a red supergiant star that has evolved off the main sequence. This means that it has bur ...
Teacher Demo: Bright Star or Close Star?
... The effects of temperature and brightness may be discussed. Betelgeuse is 15 times bigger (in radius) than Rigel and it is closer by more than 100 ly. Why is Rigel brighter? The explanation is that Betelgeuse is a red supergiant star that has evolved off the main sequence. This means that it has bur ...
... The effects of temperature and brightness may be discussed. Betelgeuse is 15 times bigger (in radius) than Rigel and it is closer by more than 100 ly. Why is Rigel brighter? The explanation is that Betelgeuse is a red supergiant star that has evolved off the main sequence. This means that it has bur ...
AST1100 Lecture Notes
... apparent and absolute magnitude. So the stars with a larger/smaller apparent magnitude also had a larger/smaller absolute magnitude. Since absolute magnitude is a measure of luminosity, what she had found was a period-luminosity relation. Pulsating stars with higher luminosity were thus found to be ...
... apparent and absolute magnitude. So the stars with a larger/smaller apparent magnitude also had a larger/smaller absolute magnitude. Since absolute magnitude is a measure of luminosity, what she had found was a period-luminosity relation. Pulsating stars with higher luminosity were thus found to be ...
Weekly Homework Questions #2, Sep. 7, 2010
... 1. What (very approximately) is the diameter of the Earth in light units? (a) less than 0.1 seconds (b) 5 seconds (c) 32 seconds (d) 3.5 minutes 2. As time goes on, why does it become increasingly difficult to communicate with deep-space probes like Voyager? (a) the time for the signal to get there ...
... 1. What (very approximately) is the diameter of the Earth in light units? (a) less than 0.1 seconds (b) 5 seconds (c) 32 seconds (d) 3.5 minutes 2. As time goes on, why does it become increasingly difficult to communicate with deep-space probes like Voyager? (a) the time for the signal to get there ...
Examples - University of Waterloo
... A photon with wavelength less than this can ionize H no matter what level the electron is initially in. ...
... A photon with wavelength less than this can ionize H no matter what level the electron is initially in. ...
Introduction to the Earth
... If the star was bigger than 30 times the mass of the sun The left over core becomes so dense that light can’t escape its gravity. Becomes a black hole. Grab any nearby matter and get bigger As matter falls in, it gives off x-rays. That’s how they find them ...
... If the star was bigger than 30 times the mass of the sun The left over core becomes so dense that light can’t escape its gravity. Becomes a black hole. Grab any nearby matter and get bigger As matter falls in, it gives off x-rays. That’s how they find them ...
Physics@Brock - Brock University
... luminosity, as well as by interferometer or eclipse measurements. • Describe the magnitude system for star brightness. ...
... luminosity, as well as by interferometer or eclipse measurements. • Describe the magnitude system for star brightness. ...
Astronomy Scavenger Hunt Distances 1. What is the
... 21. Light travels as waves, and one property of waves is their wavelength. What is a typical wavelength for radio waves? 22. What is a typical wavelength for microwaves? 23. What is a typical wavelength for infrared waves? 24. What is a typical wavelength for visible light waves? 25. What is a typi ...
... 21. Light travels as waves, and one property of waves is their wavelength. What is a typical wavelength for radio waves? 22. What is a typical wavelength for microwaves? 23. What is a typical wavelength for infrared waves? 24. What is a typical wavelength for visible light waves? 25. What is a typi ...
Solution
... 1a) Do we need Special Relativity to understand the Doppler shift of light emitted from fastmoving objects? Y 1b) If a star would pass our solar system with very high speed, there would be a Doppler shift even when it moves exactly perpendicular to our line of sight. True? Y [This is due to the time ...
... 1a) Do we need Special Relativity to understand the Doppler shift of light emitted from fastmoving objects? Y 1b) If a star would pass our solar system with very high speed, there would be a Doppler shift even when it moves exactly perpendicular to our line of sight. True? Y [This is due to the time ...
Introduction to Astronomy
... Magnitude system for brightness • Smaller numbers imply brighter stars. • “Apparent magnitude” is a measure of apparent brightness. Antares has mag. 1; Polaris has mag. 2; naked eye limit is about 6. Sirius has mag. –1.5. • “Absolute magnitude” is a measure of true brightness. It’s what the apparen ...
... Magnitude system for brightness • Smaller numbers imply brighter stars. • “Apparent magnitude” is a measure of apparent brightness. Antares has mag. 1; Polaris has mag. 2; naked eye limit is about 6. Sirius has mag. –1.5. • “Absolute magnitude” is a measure of true brightness. It’s what the apparen ...
Stars - cmamath
... Describe the life cycle of stars and be able to diagram it. Make and use an H-R diagram. Define luminosity and magnitude. ...
... Describe the life cycle of stars and be able to diagram it. Make and use an H-R diagram. Define luminosity and magnitude. ...
Classification_of_Stars_By_Luminosity
... In the nineteenth century systems were developed for measuring exactly how much light was arriving from a star. The intensity of the light (the energy arriving every second per metre 2 at Earth) was calculated. This is sometimes referred to as the apparent brightness of the star ...
... In the nineteenth century systems were developed for measuring exactly how much light was arriving from a star. The intensity of the light (the energy arriving every second per metre 2 at Earth) was calculated. This is sometimes referred to as the apparent brightness of the star ...
Problem Set # 7: The Penultimate Problem Set Due Wednesday
... 3) [20 points] We can detect a star with our naked eyes as long as its flux is above some minimum threshold, Fmin . The flux of the Sun would be equal to Fmin if it were at a distance of 17 parsecs from us. In other words, the maximum distance at which you would be able to see the Sun with your nak ...
... 3) [20 points] We can detect a star with our naked eyes as long as its flux is above some minimum threshold, Fmin . The flux of the Sun would be equal to Fmin if it were at a distance of 17 parsecs from us. In other words, the maximum distance at which you would be able to see the Sun with your nak ...
Cepheid Calibration
... The apparent brightness of a light source varies inversely as the square of its distance. In other words, if the distance between an observer and a light source is doubled, the light source will appear four times as faint to the observer. Astronomers can use this inverse square law to estimate dist ...
... The apparent brightness of a light source varies inversely as the square of its distance. In other words, if the distance between an observer and a light source is doubled, the light source will appear four times as faint to the observer. Astronomers can use this inverse square law to estimate dist ...
STARS Chapter 8 Section 1
... • The brightness(or magnitude) of a star as we see it from Earth is the star’s apparent magnitude.*** A bright star can look very dim if it is very far away from Earth. A dim star can appear bright if it is closer to Earth. • Where would you see the apparent magnitude of a star? ...
... • The brightness(or magnitude) of a star as we see it from Earth is the star’s apparent magnitude.*** A bright star can look very dim if it is very far away from Earth. A dim star can appear bright if it is closer to Earth. • Where would you see the apparent magnitude of a star? ...
Barred Spiral Galaxy
... • Large amounts of electrically charged gas are ejected suddenly from the Sun’s corona. ...
... • Large amounts of electrically charged gas are ejected suddenly from the Sun’s corona. ...
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.