Knowing the Heavens

1
Knowing the Heavens

• Chapter Two

2
Naked-eye astronomy had an important placein
ancient civilizations

• Positional astronomy
• the study of the positions of objects in the sky
  and how these positions change
• Naked-eye astronomy
• the sort that requires no equipment but human
  vision
• Extends far back in time
• British Isles Stonehenge
• Native American Medicine Wheel
• Aztec, Mayan and Incan temples
• Egyptian pyramids

3
(No Transcript)
4
Eighty-eight constellations cover the entire sky

• Ancient peoples looked at the stars and imagined
  groupings made pictures in the sky
• We still refer to many of these groupings
• Astronomers call them constellations (from the
  Latin for group of stars)

5
Modern Constellations

• On modern star charts, the entire sky is divided
  into 88 regions. Each is a constellation
• Most stars in a constellation are nowhere near
  one another
• They only appear to be close together because
  they are in nearly the same direction as seen
  from Earth

6
(No Transcript)
7
The appearance of the sky changes during the
course of the night and from one night to the next

• Stars appear to rise in the east, slowly rotate
  about the earth and set in the west.
• This diurnal or daily motion of the stars is
  actually caused by the 24-hour rotation of the
  earth.

8
(No Transcript)
9
(No Transcript)
10
Animation of constellation movement

• To represent what we have just discussed, follow
  this animation from the vantage point of our
  Californian observer.

11
Annual Motion

• The stars also appear to slowly shift in position
  throughout the year
• This is due to the orbit of the earth around the
  sun
• If you follow a particular star on successive
  evenings, you will find that it rises
  approximately 4 minutes earlier each night, or 2
  hours earlier each month

12
It is convenient to imagine that the stars are
located on a celestial sphere

• The celestial sphere is an imaginary object that
  has no basis in physical reality
• However it is still a model that remains a useful
  tool of positional astronomy
• Landmarks on the celestial sphere are projections
  of those on the Earth

13

• Celestial equator divides the sky into northern
  and southern hemispheres
• Celestial poles are where the Earths axis of
  rotation would intersect the celestial sphere
• Polaris is less than 1 away from the north
  celestial pole, which is why it is called the
  North Star or the Pole Star.
• Point in the sky directly overhead an observer
  anywhere on Earth is called that observers
  zenith.

14
The Celestial Coordinate System

• Again, let us see what we have just determined in
  a more 3-dimension manner.

15
Positional astronomy plays an important role in
keeping track of time

• Apparent solar time is based on the apparent
  motion of the Sun across the celestial sphere,
  which varies over the course of the year
• Mean solar time is based on the motion of an
  imaginary mean sun along the celestial equator,
  which produces a uniform mean solar day of 24
  hours
• Ordinary watches and clocks measure mean solar
  time
• Sidereal time is based on the apparent motion of
  the celestial sphere

16

• Local noon is defined to be when the Sun crosses
  the upper meridian, which is the half of the
  meridian above the horizon

17
(No Transcript)
18
Sidereal and Solar Days

• Appreciating the difference between a solar day
  and a sidereal day is a challenging concept. See
  if this helps.

19
Circumpolar stars

• At any time, an observer can see only half of the
  celestial sphere
• The other half is below the horizon, hidden by
  the body of the Earth

20
(No Transcript)
21
(No Transcript)
22
(No Transcript)
23
Last thought on coordinates

• The Equatorial System of Coordinates is what most
  astronomers use when specifying the location of
  an object on the Celestial Sphere
• Right Ascension (measured eastwards from the
  Vernal Equinox) goes from 0h to 24h
• Declination (measured north or south from the
  celestial equator goes from -90 to 90 .
• The hour angle (HA) of an object is the angle
  between the meridian on which the object is
  situated and the (observers) celestial meridian
• ST RA HA

24
The seasons are caused by the tilt of Earths
axis of rotation

• The Earths axis of rotation is not perpendicular
  to the plane of the Earths orbit
• It is tilted about 23½ away from the
  perpendicular is called the obliquity.
• The Earth maintains this tilt as it orbits the
  Sun, with the Earths north pole pointing toward
  the north celestial pole

25
(No Transcript)
26
The Earths orbit

• Seasons do NOT arise from the distance the Earth
  is from the Sun but rather as a result of the
  Earths annual motion and axial inclination the
  tip of our planet with respect to its orbital
  plane. As we move around the Sun, the
  orientation of our planet gives us seasons.

27
Seasons

• During part of the year the northern hemisphere
  of the Earth is tilted toward the Sun
• As the Earth spins on its axis, a point in the
  northern hemisphere spends more than 12 hours in
  the sunlight
• The days there are long and the nights are short,
  and it is summer in the northern hemisphere and
  winter in the southern hemisphere
• The summer is hot not only because of the
  extended daylight hours but also because the Sun
  is high in the northern hemispheres sky
• As a result, sunlight strikes the ground at a
  nearly perpendicular angle that heats the ground
  efficiently
• This situation reverses six months later

28
(No Transcript)
29

• The Sun appears to trace out a circular path
  called the ecliptic on the celestial sphere
  tilted at 23 ½ degrees to the equator
• The ecliptic and the celestial equator intersect
  at only two points
• Each point is called an equinox
• The point on the ecliptic farthest north of the
  celestial equator that marks the location of the
  Sun at the beginning of summer in the northern
  hemisphere is called the summer solstice
• At the beginning of the northern hemispheres
  winter the Sun is farthest south of the celestial
  equator at a point called the winter solstice

Sept 21
June 21
Dec 21
March 31
30
(No Transcript)
31
Landmarks on the Earths surface are marked by
the Suns position in the sky throughout the year
32
The Moon helps to cause precession, a slow,
conical motion of Earths axis of rotation
33
Precession causes the gradual change of the star
that marks the North Celestial Pole
34
Astronomical observations led to the development
of the modern calendar

• The day is based on the Earths rotation
• The year is based on the Earths orbit
• The month is based on the lunar cycle
• None of these are exactly the same as nature so
  astronomers use the average or mean day and leap
  years to keep the calendar and time consistent

35
The different types of year.

• The sidereal year (year with respect to the
  stars) measured in solar time is 365d 6h 9m 10s
  (365.2564d) in length.
• The tropical year (successive passages of the Sun
  through the Vernal Equinox) is 365d 5h 48m 46s
  (365.2422d) in length.
• Due to precession, the tropical year is 20m 24s
  shorter than the sidereal year.

36
Calendars

• Caesar introduced the 365.25 days calendar and
  thus the Leap Year (February 29)
• However, this is 11m 14s longer than the real
  tropical year. This accumulates to 3 days in 4
  centuries error.
• To correct, October 4 was followed by October 15,
  in 1562 and the century rule was invoked.

37
(No Transcript)
38
(No Transcript)