The life cycle of a star
... When a star nears the end of its life, it runs out of hydrogen and other fuels needed to produce energy Pressure decreases in the star so the star swells (gets bigger) and cools down (turns red) Stars equal to or smaller than the sun become red giants Stars much larger than the Sun become red ...
... When a star nears the end of its life, it runs out of hydrogen and other fuels needed to produce energy Pressure decreases in the star so the star swells (gets bigger) and cools down (turns red) Stars equal to or smaller than the sun become red giants Stars much larger than the Sun become red ...
Day-6
... http://www.ulalaunch.com/docs/product_sheet/Delt aIVPayloadPlannersGuide2007.pdf This is the Delta-IV payload guide overview. 20MB. ...
... http://www.ulalaunch.com/docs/product_sheet/Delt aIVPayloadPlannersGuide2007.pdf This is the Delta-IV payload guide overview. 20MB. ...
Stars and Their Characteristics
... variation of brightness – pulsating stars change brightness as they expand and contract – Cepheid variable- yellow supergiants whose cycles of brightness range from about 1 day to 50 days • the slower the cycle, the greater the luminosity of the star • can calculate the distances to galaxies in whic ...
... variation of brightness – pulsating stars change brightness as they expand and contract – Cepheid variable- yellow supergiants whose cycles of brightness range from about 1 day to 50 days • the slower the cycle, the greater the luminosity of the star • can calculate the distances to galaxies in whic ...
Star Life Cycle Computer Lab
... 12. What is the 3rd fuel that stars can use after Hydrogen and Helium? The Beginning of the End 13. When a star is fusing helium, what stage of its life is it considered? What type of star is this? 14. Do the helium lab and Star Quiz 2. End of a Star 15. What are the 3 possible deaths of a star? 16. ...
... 12. What is the 3rd fuel that stars can use after Hydrogen and Helium? The Beginning of the End 13. When a star is fusing helium, what stage of its life is it considered? What type of star is this? 14. Do the helium lab and Star Quiz 2. End of a Star 15. What are the 3 possible deaths of a star? 16. ...
Unit 11 Vocabulary
... 10. black hole - a place in space where gravity pulls so much that even light can’t get out. The gravity is so strong because matter has been squeezed into a tiny space. 11. Nebula - a cloud of gas and dust in space. Some nebulae are regions where new stars are being formed, while others are the rem ...
... 10. black hole - a place in space where gravity pulls so much that even light can’t get out. The gravity is so strong because matter has been squeezed into a tiny space. 11. Nebula - a cloud of gas and dust in space. Some nebulae are regions where new stars are being formed, while others are the rem ...
Document
... should swept-up equal areas in any given period of time. [1A] It means that when Halley is furthest away from the Sun, its speed must be lower than the speed it has when it is closest to the Sun. [1A] Therefore, Kc – Kf > 0。 [1A] ...
... should swept-up equal areas in any given period of time. [1A] It means that when Halley is furthest away from the Sun, its speed must be lower than the speed it has when it is closest to the Sun. [1A] Therefore, Kc – Kf > 0。 [1A] ...
Measuring the ligth
... We have seen how the flux received on earth depended strongly on the object’s distance, more precisely according to the inverse of the squared distance. The intensity, I, however is of great interest because it doesn’t depend on the distance. Effectively, the true area at the source is that of a sol ...
... We have seen how the flux received on earth depended strongly on the object’s distance, more precisely according to the inverse of the squared distance. The intensity, I, however is of great interest because it doesn’t depend on the distance. Effectively, the true area at the source is that of a sol ...
Answers to Coursebook questions – Chapter E3
... From the HR diagram a main sequence star at this temperature has a luminosity that is about 100 times larger than the Sun’s, i.e. 3.9 10 28 W . ...
... From the HR diagram a main sequence star at this temperature has a luminosity that is about 100 times larger than the Sun’s, i.e. 3.9 10 28 W . ...
AST121 Introduction to Astronomy
... • A graph of stars’ luminosity (or absolute magnitude since they are related) vs. temperature (or spectral type since they are related) • short for Hertzsprung-Russell diagram ...
... • A graph of stars’ luminosity (or absolute magnitude since they are related) vs. temperature (or spectral type since they are related) • short for Hertzsprung-Russell diagram ...
Parallax - High Point University
... • A graph of stars’ luminosity (or absolute magnitude since they are related) vs. temperature (or spectral type since they are related) • short for Hertzsprung-Russell diagram ...
... • A graph of stars’ luminosity (or absolute magnitude since they are related) vs. temperature (or spectral type since they are related) • short for Hertzsprung-Russell diagram ...
Measuring the Stars
... the main sequence, as this is where most stars are. Also indicated is the white dwarf region; these stars are hot but not very luminous, as they are quite small. ...
... the main sequence, as this is where most stars are. Also indicated is the white dwarf region; these stars are hot but not very luminous, as they are quite small. ...
Stars
... the Big Dipper. It was the first binary star system to be imaged with a telescope. Spectroscopic observations show periodic Doppler shifts in the spectra of Mizar A and B, indicating that they are each binary stars. But they were too close to be directly imaged - until 2 May 1996, when the NPOI prod ...
... the Big Dipper. It was the first binary star system to be imaged with a telescope. Spectroscopic observations show periodic Doppler shifts in the spectra of Mizar A and B, indicating that they are each binary stars. But they were too close to be directly imaged - until 2 May 1996, when the NPOI prod ...
Stars: flux, luminosity, color, and temperature
... `magnitude’ groups according to how bright they looked to his eye. • Herschel (1800s) first measured the brightness of stars quantitatively and matched his measurements onto Ptolemy’s magnitude groups and assigned a number for the magnitude of each star. ...
... `magnitude’ groups according to how bright they looked to his eye. • Herschel (1800s) first measured the brightness of stars quantitatively and matched his measurements onto Ptolemy’s magnitude groups and assigned a number for the magnitude of each star. ...
Lecture 24 - Empyrean Quest Publishers
... How bright (L in watts)? Luminosity at the source is determined from apparent brightness and distance (d). Apparent magnitude (old way). We can see about 1,000 stars in Northern Hemisphere with naked eye. Hipparchus rated them from 1 to 6. A '1' is 2.52 x brighter than a '2', etc. Range in brightnes ...
... How bright (L in watts)? Luminosity at the source is determined from apparent brightness and distance (d). Apparent magnitude (old way). We can see about 1,000 stars in Northern Hemisphere with naked eye. Hipparchus rated them from 1 to 6. A '1' is 2.52 x brighter than a '2', etc. Range in brightnes ...
Review3-2016
... How do we use the atomic emission and absorption spectra to find the composition of a star? How do we determine the rotation period of a star? How do we determine the distance to a star using Stellar Parallax? What is an H-R diagram and what information does it give us? One of the Ca spectral lines ...
... How do we use the atomic emission and absorption spectra to find the composition of a star? How do we determine the rotation period of a star? How do we determine the distance to a star using Stellar Parallax? What is an H-R diagram and what information does it give us? One of the Ca spectral lines ...
The Hertzsprung – Russell Diagram
... For astronomers, a graph that displays a star’s luminosity on the y-axis and its surface temperature on the x-axis sets up an extremely useful diagram called a Hertzsprung-Russell, or H-R Diagram. In 1910 Ejnar Hertzsprung and Henry Norris Russell discovered that when all of the known stars were put ...
... For astronomers, a graph that displays a star’s luminosity on the y-axis and its surface temperature on the x-axis sets up an extremely useful diagram called a Hertzsprung-Russell, or H-R Diagram. In 1910 Ejnar Hertzsprung and Henry Norris Russell discovered that when all of the known stars were put ...
Answers to Coursebook questions – Chapter E2
... The HR diagram is a plot of luminosity (or absolute magnitude) on the vertical axis and temperature (increasing to the left) on the horizontal axis. The horizontal axis may be also be labelled by the spectral class of the star. The diagram shows three major groupings of stars. Main sequence stars oc ...
... The HR diagram is a plot of luminosity (or absolute magnitude) on the vertical axis and temperature (increasing to the left) on the horizontal axis. The horizontal axis may be also be labelled by the spectral class of the star. The diagram shows three major groupings of stars. Main sequence stars oc ...
solutions
... surface brightness in turn yield the star’s luminosity (its total light output, or absolute magnitude) and often its evolutionary status (young, middle-aged, or nearing death). The luminosity (when compared to the star’s apparent brightness in our sky) also gives a good idea of the star’s distance. ...
... surface brightness in turn yield the star’s luminosity (its total light output, or absolute magnitude) and often its evolutionary status (young, middle-aged, or nearing death). The luminosity (when compared to the star’s apparent brightness in our sky) also gives a good idea of the star’s distance. ...
E8B6_CRT_CR_MSTIPS_Final
... A. Using apparent magnitude, identify the brightest star and the dimmest star. Then, using absolute magnitude, identify the brightest star and the dimmest star B. Perform the following calculations. i. Determine the absolute magnitude for the star with the brightest apparent magnitude and calculate ...
... A. Using apparent magnitude, identify the brightest star and the dimmest star. Then, using absolute magnitude, identify the brightest star and the dimmest star B. Perform the following calculations. i. Determine the absolute magnitude for the star with the brightest apparent magnitude and calculate ...
FINAL EXAM Name: ASTRONOMY II - 79202 Spring 1995
... using Doppler shift spectroscopy. They found a rotation speed of 550 km/sec within 0.2” on either side of the center of the disk. The mass within this region is A. At least one solar mass. B. 2 1033 kg C. 2 1039 kg D. 4 1044 kg E. There is not enough information to determine the mass. 18. Elec ...
... using Doppler shift spectroscopy. They found a rotation speed of 550 km/sec within 0.2” on either side of the center of the disk. The mass within this region is A. At least one solar mass. B. 2 1033 kg C. 2 1039 kg D. 4 1044 kg E. There is not enough information to determine the mass. 18. Elec ...
NAME:______ANSWER KEY_______________________Period
... 2. What does light year measure? distance 3. Why do we use light year instead of kilometers? Kilometers would be way to big of a number 4. Change the following number 78,000,000 to scientific notation. 7.8 x 107 5. Write 1.90 x 108 in standard number form. 190,000,000 6. Define Nebula: a large cloud ...
... 2. What does light year measure? distance 3. Why do we use light year instead of kilometers? Kilometers would be way to big of a number 4. Change the following number 78,000,000 to scientific notation. 7.8 x 107 5. Write 1.90 x 108 in standard number form. 190,000,000 6. Define Nebula: a large cloud ...
Boötes
Boötes /boʊˈoʊtiːz/ is a constellation in the northern sky, located between 0° and +60° declination, and 13 and 16 hours of right ascension on the celestial sphere. The name comes from the Greek Βοώτης, Boōtēs, meaning herdsman or plowman (literally, ox-driver; from βοῦς bous “cow”). The ""ö"" in the name is a diaeresis, not an umlaut, meaning that each 'o' is to be pronounced separately.One of the 48 constellations described by the 2nd century astronomer Ptolemy, Boötes is now one of the 88 modern constellations. It contains the fourth brightest star in the night sky, the orange-hued Arcturus. Boötes is home to many other bright stars, including eight above the fourth magnitude and an additional 21 above the fifth magnitude, making a total of 29 stars easily visible to the naked eye.