Presentation on theme: "Slide 1 2.Motions on the sky: The celestial sphere."— Presentation transcript:
Slide 1 2.Motions on the sky: The celestial sphere
Slide 2 Star trails
Slide 3 The diurnal motion
Slide 4 The diurnal motion The entire sky appears to turn around imaginary points in the northern and southern sky once in 24 hours. This is termed the daily or diurnal motion of the celestial sphere, and is in reality a consequence of the daily rotation of the earth on its axis. The diurnal motion affects all objects in the sky and does not change their relative positions: the diurnal motion causes the sky to rotate as a whole once every 24 hours. Superposed on the overall diurnal motion of the sky is "intrinsic" motion that causes certain objects on the celestial sphere to change their positions with respect to the other objects on the celestial sphere. These are the "wanderers" of the ancient astronomers: the planets, the Sun, and the Moon.
Slide 5 We can define a useful coordinate system for locating objects on the celestial sphere by projecting onto the sky the latitude- longitude coordinate system that we use on the surface of the earth. The stars rotate around the North and South Celestial Poles. These are the points in the sky directly above the geographic north and south pole, respectively. The Earth's axis of rotation intersects the celestial sphere at the celestial poles. The number of degrees the celestial pole is above the horizon is equal to the latitude of the observer. Fortunately, for those in the northern hemisphere, there is a fairly bright star real close to the North Celestial Pole (Polaris or the North star). Another important reference marker is the celestial equator: an imaginary circle around the sky directly above the Earth's equator. It is always 90 degrees from the poles. All the stars rotate in a path that is parallel to the celestial equator. The celestial equator intercepts the horizon at the points directly east and west anywhere on the Earth. The celestial sphere
Slide 7 Latitude
Slide 10 The arc that goes through the north point on the horizon, zenith, and south point on the horizon is called the meridian. The positions of the zenith and meridian with respect to the stars will change as the celestial sphere rotates and if the observer changes locations on the Earth, but those reference marks do not change with respect to the observer's horizon. Any celestial object crossing the meridian is at its highest altitude (distance from the horizon) during that night (or day). The angle the star paths make with respect to the horizon = 90 degrees - (observer's latitude). During daylight, the meridian separates the morning and afternoon positions of the Sun. In the morning the Sun is ``ante meridiem'' (Latin for ``before meridian'') or east of the meridian, abbreviated ``a.m.''. At local noon the Sun is right on the meridian. At local noon the Sun is due south for northern hemisphere observers and due north for southern hemisphere observers. In the afternoon the Sun is ``post meridiem'' (Latin for ``after meridian'') or west of the meridian, abbreviated ``p.m.''.
Slide 12 If you are in the northern hemisphere, celestial objects north of the celestial equator are above the horizon for more than 12 hours because you see more than half of their total 24-hour path around you. Celestial objects on the celestial equator are up 12 hours and those south of the celestial equator are above the horizon for less than 12 hours because you see less than half of their total 24-hour path around you. The opposite is true if you are in the southern hemisphere. Notice that stars closer to the NCP are above the horizon longer than those farther away from the NCP. Those stars within an angular distance from the NCP equal to the observer's latitude are above the horizon for 24 hours---they are circumpolar stars. Also, those stars close enough to the SCP (within a distance = observer's latitude) will never rise above the horizon. They are also called circumpolar stars.
Slide 14 p. 16
Slide 15 Star trails around South Celestial Pole (Gemini Observatory, Chile)
Slide 18 Here is a summary of the positions of the celestial reference marks (note that ``altitude'' means the number of degrees above the horizon): Meridian always goes through due North, zenith, and due South points. Altitude of zenith = 90° (straight overhead) always. Altitude of celestial pole = observer's latitude. Observers in northern hemisphere see NCP; observers in southern hemisphere see SCP. Altitude of celestial equator on meridian = 90 - observer's latitude. Celestial equator always intercepts horizon at exactly East and exactly West points. Angle celestial equator (and any star path) makes with horizon = 90 - observer's latitude. Stars move parallel to the celestial equator.
Slide 19 This angle = 90 o – Latitude!
Slide 20 Measuring distances on the sphere
Slide 21 p. 17 To measure distances on the imaginary celestial sphere, you use ``angles on the sky'' instead of meters or kilometers. There are 360 degrees in a full circle and 90 degrees in a right angle (two perpendicular lines intersecting each other make a right angle). Each degree is divided into 60 minutes of arc. A quarter viewed face-on from across the length of a football field is about 1 arc minute across. Each minute of arc is divided into 60 seconds of arc. The ball in the tip of a ballpoint pen viewed from across the length of a football field is about 1 arc second across. The Sun and Moon are both about 0.5 degrees = 30 arc minutes in diameter. The pointer stars in the bowl of the Big Dipper are about 5 degrees apart and the bowl of the Big Dipper is about 30 degrees from the NCP. The arc from the north point on the horizon to the point directly overhead to the south point on the horizon is 180 degrees, so any object directly overhead is 90 degrees above the horizon and any object ``half-way up'' in the sky is about 45 degrees above the horizon. 1 degree = 60 arcmin = 3600 arcsec 180 degrees = radian
Slide 22 The "Road of the Sun" on the Celestial Sphere 1.Diurnal motion from east to west due to the earth’s spinning around its axis, with ~ 24 h period 2.Drift eastward with respect to the stars ~ 1 degree per day with the period of ~ days
Slide 24 Ecliptic and Zodiac Sun travels 360 o / days ~ 1 o /day
Slide 25 axis As a result, planes of the ecliptic and celestial equator make an angle 23.5 o Celestial equator
Slide 26 p. 22
Slide 27 The ecliptic and celestial equator intersect at two points: the vernal (spring) equinox and autumnal (fall) equinox. The Sun crosses the celestial equator moving northward at the vernal equinox around March 21 and crosses the celestial equator moving southward at the autumnal equinox around September 22. When the Sun is on the celestial equator at the equinoxes, everybody on the Earth experiences 12 hours of daylight and 12 hours of night for those two days (hence, the name ``equinox'' for ``equal night''). The day of the vernal equinox marks the beginning of the three-month season of spring on our calendar and the day of the autumn equinox marks the beginning of the season of autumn (fall) on our calendar. On those two days of the year, the Sun will rise in the exact east direction, follow an arc right along the celestial equator and set in the exact west direction.
Slide 28 When the Sun is above the celestial equator during the seasons of spring and summer, you will have more than 12 hours of daylight. The Sun will rise in the northeast, follow a long, high arc north of the celestial equator, and set in the northwest. Where exactly it rises or sets and how long the Sun is above the horizon depends on the day of the year and the latitude of the observer. When the Sun is below the celestial equator during the seasons of autumn and winter, you will have less than 12 hours of daylight. The Sun will rise in the southeast, follow a short, low arc south of the celestial equator, and set in the southwest. The exact path it follows depends on the date and the observer's latitude.
Slide 29 Drawn for northern latitudes, these are the paths the sun takes across the sky on the equinoxes and solstices. Can you see that the summer path is longer (and therefore that the summer sun stays in the sky longer)?
Slide 30 Solstices
Slide 31 Since the ecliptic is tilted 23.5 degrees with respect to the celestial equator, the Sun's maximum angular distance from the celestial equator is 23.5 degrees. This happens at the solstices. For observers in the northern hemisphere, the farthest northern point above the celestial equator is the summer solstice, and the farthest southern point is the winter solstice. The word ``solstice'' means ``sun standing still'' because the Sun stops moving northward or southward at those points on the ecliptic. The Sun reaches winter solstice around December 21 and you see the least part of its diurnal path all year---this is the day of the least amount of daylight and marks the beginning of the season of winter for the northern hemisphere. On that day the Sun rises at its furthest south position in the southeast, follows its lowest arc south of the celestial equator, and sets at its furthest south position in the southwest. The Sun reaches the summer solstice around June 21 and you see the greatest part of its diurnal path above the horizon all year---this is the day of the most amount of daylight and marks the beginning of the season of summer for the northern hemisphere. On that day the Sun rises at its furthest north position in the northeast, follows its highest arc north of the celestial equator, and sets at its furthest north position in the northwest.
Slide 32 The axis tilt causes the seasons!!
Slide 33 p. 22
Slide 34 p. 23 Longer day
Slide 35 p. 23 Shorter day
Slide 36 p. 23
Slide 37 There are no seasons on the equator (except for the changes related to weather) In reality the seasons “lag”: for example, maximum summer temperatures occur ~ 1 month later than the summer solstice. Blame oceans that act as storages of heat!
Slide 38 Seasons - summary 1.Seasons are NOT caused by varying distances from the Earth to the Sun 2.The primary cause of seasons is the 23.5 degree tilt of the Earth's rotation axis with respect to the plane of the ecliptic. Note: the Earth is actually closest to the Sun in January 4! The Seasons in the Northern Hemisphere Perihelion: × 10 6 km; Aphelion: × 10 6 km
Slide 39 Thus, we experience Summer in the Northern Hemisphere when the Earth is on that part of its orbit where the N. Hemisphere is oriented more toward the Sun and therefore: 1.the Sun rises higher in the sky and is above the horizon longer, 2.The rays of the Sun strike the ground more directly. Likewise, in the N. Hemisphere Winter the hemisphere is oriented away from the Sun, the Sun only rises low in the sky, is above the horizon for a shorter period, and the rays of the Sun strike the ground more obliquely.
Slide 40 Keeping track of time …
Slide 42 Solar and Sidereal Day The fact that our clocks are based on the solar day (24 hours) and the Sun appears to drift eastward with respect to the stars (or lag behind the stars) by about 1 degree per day means that if you look closely at the positions of the stars over a period of several days, you will notice that according to our clocks, the stars rise and set 4 minutes earlier each day. Our clocks say that the day is 24 hours long, so the stars move around the Earth in 23 hours 56 minutes. This time period is called the sidereal day because it is measured with respect to the stars. This is the true rotation rate of the Earth and stays the same no matter where the Earth is in its orbit---the sidereal day = 23 hours 56 minutes on every day of the year. One month later (30 days) a given star will rise 2 hours earlier than it did before (30 days × 4 minutes/day = 120 minutes). A year later that star will rise at the same time as it did today.
Slide 43 Precession of the rotation axis
Slide 44 Precession causes the north celestial pole to drift among the stars, completing a circle in 26,000 years.
Slide 45 Sidereal and tropical year The precession of the Earth's rotation axis introduces another difference between sidereal time and solar time. This is seen in how the year is measured. A year is defined as the orbital period of the Earth. However, if you use the Sun's position as a guide, you come up with a time interval about 20 minutes shorter than if you use the stars as a guide. The time required for the constellations to complete one 360° cycle around the sky and to return to their original point on our sky is called a sidereal year. This is the time it takes the Earth to complete exactly one orbit around the Sun and equals solar days. The slow shift of the star coordinates from precession means that the Sun will not be at exactly the same position with respect to the celestial equator after one sidereal year. The tropical year is the time interval between two successive vernal equinoxes. It equals solar days and is the year our calendars are based on. After several thousand years the 20 minute difference between sidereal and tropical years would have made our summers occur several months earlier if we used a calendar based on the sidereal year.
Slide 46 There is a further complication in that the actual Sun's drift against the stars is not uniform. Apparent solar time is based on the component of the Sun's motion parallel to the celestial equator. This effect alone would account for as much as 9 minutes difference between the actual Sun and a fictional mean Sun moving uniformily along the celestial equator.
Slide 48 Actual motion of the sun and fictitious uniformly moving mean sun
Slide 49 Myr ago Puzzle: Ice Ages! Occur with a period of ~ 250 million yr Cycles of glaciation within the ice age occur with a period of 40,000 yr Most recent ice age began ~ 3 million yr ago and is still going on!
Slide 50 Last Glacial Maximum: 18,000 yr ago 32% of land covered with ice Sea level 120 m lower than now
Slide 52 Ice Ages - cause Atmospheric composition, especially greenhouse gases and dust; Changes in the Earth’s orbit and inclination; The motion of tectonic plates resulting in changes in the landmass distribution; Variations in the solar output; The impact of large meteorites; Eruptions of supervolcanoes
Slide 53 Cycles of glaciation - cause Theory: cyclic climate changes due to variations in the Earth’s orbital parameters –Precession (26,000 yr cycle) –Eccentricity (varies from 0.00 to 0.06 with 100,000 and 400,000 yr cycles) –Axis tilt (varies from 24.5 o to 22.1 o with 41,000 yr cycle Milutin Milankovitch 1920
Slide 55 Varies from 0.00 to 0.06 (currently 0.017) Periodicity 100,000 and 400,000 yr Eccentricity cycle modulates the amplitude of the precession cycle
Slide 57 An effect called precession causes the Sun's vernal equinox point to slowly shift westward over time, so a star's RA and dec will slowly change by about 1.4 degrees every century (a fact ignored by astrologers), or about 1 minute increase in a star's RA every twenty years. This is caused by the gravitational pulls of the Sun and Moon on the Earth's equatorial bulge (from the Earth's rapid rotation) in an effort to reduce the tilt of the Earth's axis with respect to the ecliptic and the plane of the Moon's orbit around the Earth (that is itself slightly tipped with respect to the ecliptic).
Slide 58 26,000 yr cycle
Slide 59 As a result, the flux of solar radiation received by the Earth oscillates with different periodicities and amplitudes This triggers changes in climate Our Earth makes a complicated motion through space, like a crazy spaceship
Slide 60 f1 f2 f3 f1+f2 f1+f2+f3 Adding oscillations with different phases and incommensurate frequencies f1 = sin[2 t + 1] f2 = 0.7 sin[3.1 t + 2.4] f3 = 1.3 sin[4.5 t + 0.3]
Slide 61 Adding Milankovitch cycles of solar irradiation for 65 degree North latitude (Berger 1991) Note the last peak 9,000 years ago when the last large ice sheet melted
Slide 62 Very good agreement in general, but some findings are still contradictory Myr ago The response of the climate system to external variations is highly nonlinear: small external variations can trigger large changes in climate. Example: ice-albedo positive feedback loop.
Slide 63 Are these effects enough to explain the Ice Ages??? Other factors? Volcanic winters, impacts, … 71,000 yr ago: eruption of Mount Toba (Sumatra) 2,800 km 3 of material thrown in the atmosphere Instant ice age? Meteorite impacts; Mass extinctions
Slide 64 Meteorite impacts – Mass extinctions and abrupt climate changes – Meteorite hypothesis –KT boundary 65 million yr ago (Cretacious-Tertiary mass extinction): 200-km impact crater near Yukatan, Mexico –PT boundary 251 million yr ago: largest extinction 90% of marine and 70% of land species extinct 200 km diameter impact crater just found offshore the northwestern Australia Role of climate changes in the development of hominids?