Coordinates and Time - University of Florida Astronomy
... The modern standard time is based upon the SI second, which is defined in terms of the oscillations for a particular transition of 133Cs rather than astronomical measures. One second = 9192631770 oscillations. IAT is effectively the atomic equivalent of UT, based upon atomic clocks instead of mean s ...
... The modern standard time is based upon the SI second, which is defined in terms of the oscillations for a particular transition of 133Cs rather than astronomical measures. One second = 9192631770 oscillations. IAT is effectively the atomic equivalent of UT, based upon atomic clocks instead of mean s ...
Ellipses, Parallax, and Retrograde Motion – Study Guide
... 3. Discuss the difference between what we see (apparent) and what is real (actual) with relation to retrograde motion or parallax. Apparent means what we see when we make our observations. Actual means what really happens as if observed from outside the solar system. For example, stars do NOT really ...
... 3. Discuss the difference between what we see (apparent) and what is real (actual) with relation to retrograde motion or parallax. Apparent means what we see when we make our observations. Actual means what really happens as if observed from outside the solar system. For example, stars do NOT really ...
sidereal day
... •It is a system of timekeeping used by astronomers, useful because a star rises and sets at the same sidereal time every day, but not at the same solar (synodic) time which is our typical time system. •Because local sidereal time is the right ascension (RA) of a star on the observers meridian, it is ...
... •It is a system of timekeeping used by astronomers, useful because a star rises and sets at the same sidereal time every day, but not at the same solar (synodic) time which is our typical time system. •Because local sidereal time is the right ascension (RA) of a star on the observers meridian, it is ...
ppt - Faculty Virginia
... In the Summer, the Sun is well north of the celestial equator and behaves more like a star near the north celestial pole (more like a circumpolar star) – so it is above the horizon much more than 12 hours. ...
... In the Summer, the Sun is well north of the celestial equator and behaves more like a star near the north celestial pole (more like a circumpolar star) – so it is above the horizon much more than 12 hours. ...
The sun, yellow dwarf star at the heart of the solar system
... at least 200 billion stars. More specifically, our sun is in a spiral arm of the galaxy called the Orion Spur. From there, the sun orbits the center of the Milky Way, bringing the planets, asteroids, comets and other objects along with it. Our solar system is moving with an average velocity of 450,00 ...
... at least 200 billion stars. More specifically, our sun is in a spiral arm of the galaxy called the Orion Spur. From there, the sun orbits the center of the Milky Way, bringing the planets, asteroids, comets and other objects along with it. Our solar system is moving with an average velocity of 450,00 ...
Lecture3
... Earth’s Rotation (once per day) causes sun/ stars/etc. to rise, transit at their highest point at the meridian, and then set. Zenith is the point directly overhead. Stars you see depends on your latitude. Some stars are always up: they are circumpolar. Constellations: Just random groupings of stars ...
... Earth’s Rotation (once per day) causes sun/ stars/etc. to rise, transit at their highest point at the meridian, and then set. Zenith is the point directly overhead. Stars you see depends on your latitude. Some stars are always up: they are circumpolar. Constellations: Just random groupings of stars ...
January 14 - Astronomy
... Florida is closer to the equator and a space shuttle just sitting on the launch pad is moving about 1,550 km/hr. If we moved the launch pad to Maine, the space shuttle sitting on the launch pad is only moving 1,275 km/hr or about 275 km/hr less than in Florida. To launch the space shuttle in Maine ...
... Florida is closer to the equator and a space shuttle just sitting on the launch pad is moving about 1,550 km/hr. If we moved the launch pad to Maine, the space shuttle sitting on the launch pad is only moving 1,275 km/hr or about 275 km/hr less than in Florida. To launch the space shuttle in Maine ...
ASTRONOMY
... B. Using the diagram answer the following questions. a. The angle of the North Star above the horizon. b. The angle between the North Star and the Celestial equator. c. The angle between the Ecliptic and Celestial equator. d. Where to find planets. e. Where to find the sun. f. Where to find the cons ...
... B. Using the diagram answer the following questions. a. The angle of the North Star above the horizon. b. The angle between the North Star and the Celestial equator. c. The angle between the Ecliptic and Celestial equator. d. Where to find planets. e. Where to find the sun. f. Where to find the cons ...
Unit 8 Chapter 29
... E=mc2 Energy = mass x the speed of light squared Because the star is a place of intense heat and pressure, the atoms are torn apart into their component nuclei and electrons. By using Einstein's equation, astronomers were able to explain the huge quantities of energy produced by the sun. The sun cha ...
... E=mc2 Energy = mass x the speed of light squared Because the star is a place of intense heat and pressure, the atoms are torn apart into their component nuclei and electrons. By using Einstein's equation, astronomers were able to explain the huge quantities of energy produced by the sun. The sun cha ...
What do we see? Stars Sun Moon Planets How do we organize
... Diurnal—rises in the east and sets in the west (reason: Earth rotates on its axis) Annual—moves through the zodiac from west to east (reason: Earth revolves in its orbit) Seasonal—rises higher in the sky at noon in summer and lower in winter. It rises above the horizon north of east in summer and so ...
... Diurnal—rises in the east and sets in the west (reason: Earth rotates on its axis) Annual—moves through the zodiac from west to east (reason: Earth revolves in its orbit) Seasonal—rises higher in the sky at noon in summer and lower in winter. It rises above the horizon north of east in summer and so ...
The Rotational Period of the Sun (Higher Level)
... calculated by using its spectrum. Stars like the Sun often show strong hydrogen emission lines such as Hα, Hβ and Hγ (below). By measuring the wavelengths of these observed lines and comparing them to their rest wavelengths we can tell whether the part of the Sun we are looking at is redshifted or b ...
... calculated by using its spectrum. Stars like the Sun often show strong hydrogen emission lines such as Hα, Hβ and Hγ (below). By measuring the wavelengths of these observed lines and comparing them to their rest wavelengths we can tell whether the part of the Sun we are looking at is redshifted or b ...
VARIOUS MEASUREMENTS OF TIME
... Since the earth rotates on its axis from west to east, all heavenly bodies (i.e. the sun and the fixed stars) appear to revolve from east to west (i.e. in clock-wise direction) around the earth. Such motion of the heavenly bodies is known as apparent motion. We may consider the earth to turn on it a ...
... Since the earth rotates on its axis from west to east, all heavenly bodies (i.e. the sun and the fixed stars) appear to revolve from east to west (i.e. in clock-wise direction) around the earth. Such motion of the heavenly bodies is known as apparent motion. We may consider the earth to turn on it a ...
Solar System Test 16-17
... 8. In the morning, Sandra notices that the sun appears on one side of the sky. In the evening she notices that the Sun appears to be on the other side of the sky. However, in class, Sandra learned that the Sun does not actually move across the sky from one side to another. Why does the sun appear to ...
... 8. In the morning, Sandra notices that the sun appears on one side of the sky. In the evening she notices that the Sun appears to be on the other side of the sky. However, in class, Sandra learned that the Sun does not actually move across the sky from one side to another. Why does the sun appear to ...
Physics 20 Lesson 23 Orbits and Satellites
... In Lesson 13 we learned about projectiles – where the vertical and horizontal components of motion act independently. For the projectile problems we worked with there was an unstated assumption that the Earth was flat. However, we know that the Earth is in fact spherical, although not perfectly so. ...
... In Lesson 13 we learned about projectiles – where the vertical and horizontal components of motion act independently. For the projectile problems we worked with there was an unstated assumption that the Earth was flat. However, we know that the Earth is in fact spherical, although not perfectly so. ...
The Sun and Its Solar System Topic 1
... thick and appears to be made of millions of individual cells, called granules about 1500 km across with a bright center and dark edges. Granules are the tops of the columns of gases that form in the region below the photosphere. The gases are rising at the centre of the granule and sinking back down ...
... thick and appears to be made of millions of individual cells, called granules about 1500 km across with a bright center and dark edges. Granules are the tops of the columns of gases that form in the region below the photosphere. The gases are rising at the centre of the granule and sinking back down ...
CHAPTER 6 THE CELESTIAL SPHERE
... While it is useful to know the hour angle of a star at a particular time for a particular observer, we still need a coordinate that is fixed on the celestial sphere. To do this, we refer to a point on the celestial equator, which I shall define more precisely later on, denoted on figure VI.2 by the ...
... While it is useful to know the hour angle of a star at a particular time for a particular observer, we still need a coordinate that is fixed on the celestial sphere. To do this, we refer to a point on the celestial equator, which I shall define more precisely later on, denoted on figure VI.2 by the ...
chapter01 - California State University, Long Beach
... Copernicus, Galileo and Newton and about when they lived. Kepler's laws and their use. The Kelvin Temperature scale. This chapter introduces some important ideas that will be needed later, such as parallax (also described in Chapter 12), angular size (also discussed in Chapter 6), and Kepler's third ...
... Copernicus, Galileo and Newton and about when they lived. Kepler's laws and their use. The Kelvin Temperature scale. This chapter introduces some important ideas that will be needed later, such as parallax (also described in Chapter 12), angular size (also discussed in Chapter 6), and Kepler's third ...
The Sun (Nearest Star to us)
... observable magnetic activity on the Sun’s surface. Because of their cooler temperature region at the magnetic region it appears as a dark spot. The temperature of the sunspot is of the order of 4250K as compared to surrounding of 5700 K. It has a inside dark part known as umbra and outside lighter p ...
... observable magnetic activity on the Sun’s surface. Because of their cooler temperature region at the magnetic region it appears as a dark spot. The temperature of the sunspot is of the order of 4250K as compared to surrounding of 5700 K. It has a inside dark part known as umbra and outside lighter p ...
Slide 1
... Sunspots are dark splotches on the face of the Sun. They are typically about 2,000 degrees Kelvin cooler than the average temperature on the photosphere. This makes them appear to be dark in comparison to their very bright surroundings. Following long-lived sunspots through time allows one to determ ...
... Sunspots are dark splotches on the face of the Sun. They are typically about 2,000 degrees Kelvin cooler than the average temperature on the photosphere. This makes them appear to be dark in comparison to their very bright surroundings. Following long-lived sunspots through time allows one to determ ...
Lecture 3 - Purdue University
... – When the Sun crosses the local meridian (reaches highest point), it is noon – Tomorrow when it does that again, it is noon again – But this day length varies (more than 24 h around Jan. 1, less than 24 h around Sept. 1) ...
... – When the Sun crosses the local meridian (reaches highest point), it is noon – Tomorrow when it does that again, it is noon again – But this day length varies (more than 24 h around Jan. 1, less than 24 h around Sept. 1) ...
The Sun: Our Extraordinary Ordinary Star
... Solar Activities and Communication • Solar activity associated with sun spots result in massive amounts of radiation and charged particles being ejected into space. • When this material overwhelms the protective Van Allen Belt layer of our atmosphere all electromagnetic activities can be interrupt ...
... Solar Activities and Communication • Solar activity associated with sun spots result in massive amounts of radiation and charged particles being ejected into space. • When this material overwhelms the protective Van Allen Belt layer of our atmosphere all electromagnetic activities can be interrupt ...
Stellar aberration
... for predicting phenomena associated with relative positions of central and planetary bodies. However, they cannot give correct results if used to determine real parameters of the macro bodies or their paths. All cosmic bodies, except stable galaxies, have translational motions in space [1]. Currentl ...
... for predicting phenomena associated with relative positions of central and planetary bodies. However, they cannot give correct results if used to determine real parameters of the macro bodies or their paths. All cosmic bodies, except stable galaxies, have translational motions in space [1]. Currentl ...
Daily "Motions" of the Celestial Sphere
... A solar day is 24 hrs -- one rotation of the Earth with respect to the Sun. Due to the Earth’s physical rotation, the celestial sphere appears to rotate around the north celestial pole - the projection of Earth's rotation axis onto the sky. The celestial sphere “completes” one rotation in a sidereal ...
... A solar day is 24 hrs -- one rotation of the Earth with respect to the Sun. Due to the Earth’s physical rotation, the celestial sphere appears to rotate around the north celestial pole - the projection of Earth's rotation axis onto the sky. The celestial sphere “completes” one rotation in a sidereal ...
Equation of time
The equation of time describes the discrepancy between two kinds of solar time. These are apparent solar time, which directly tracks the motion of the sun, and mean solar time, which tracks a fictitious ""mean"" sun with noons 24 hours apart. Apparent (or true) solar time can be obtained by measurement of the current position (hour angle) of the Sun, or indicated (with limited accuracy) by a sundial. Mean solar time, for the same place, would be the time indicated by a steady clock set so that over the year its differences from apparent solar time average to zero.The equation of time is the east or west component of the analemma, a curve representing the angular offset of the Sun from its mean position on the celestial sphere as viewed from Earth. The equation of time values for each day of the year, compiled by astronomical observatories, were widely listed in almanacs and ephemerides.