the sky
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0. Note that the following lectures include animations and PowerPoint effects such as fly-ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). 0. The Sky. Chapter 2. 0. Guidepost. - PowerPoint PPT PresentationTRANSCRIPT
Note that the following lectures include
animations and PowerPoint effects such as
fly-ins and transitions that require you to be
in PowerPoint's Slide Show mode
(presentation mode).
The SkyChapter 2
The previous chapter took you on a cosmic zoom through space and time. That quick preview sets the stage for the drama to come. In this chapter you can view the sky from Earth with your own eyes, and as you do, consider four important questions:
•How do astronomers name stars and compare their brightness?
•How do Earth’s motions affect the appearance of the sky?
•What causes the seasons?
•How can astronomical cycles affect Earth’s climate?
As you study the sky and its motions, you will be thinking of Earth as a planet rotating on its axis and moving in an orbit. The next chapter will introduce you to other impressive sky cycles: phases of the moon and eclipses.
Guidepost
I. The StarsA. ConstellationsB. The Names of the StarsC. Favorite StarsD. The Brightness of StarsE. Magnitude and Flux
II. The Sky and Celestial MotionA. The Celestial SphereB. Precession
III. The Cycles of the SunA. The Annual Motion of the SunB. The Seasons
C. The Motion of the Planets
Outline
V. Astronomical Influences on Earth's ClimateA. The HypothesisB. The Evidence
Outline (continued)
Constellations
In ancient times, constellations only referred to the brightest stars that appeared to form groups.
Constellations (2)
They were believed to represent great heroes and mythological figures. Their position in the sky
seemed to tell stories that were handed down from generation to generation over thousands of years.
Constellations (3)
Today, constellations are well-defined regions on the sky, irrespective of the presence or absence of bright stars in those regions.
Constellations (4)The stars of a constellation
only appear to be close to one
another.
Usually, this is only a projection
effect:
The stars of a constellation
may be located at very different distances from
us.
Constellations (5)Stars are named by a Greek letter () according to their relative brightness within a given constellation +
the possessive form of the name of the constellation:
Orion
Betelgeuse
Rigel
Rigel = OrionisBetelgeuse = Orionis
Constellations (6)
Some examples of easily recognizable constellations and their brightest stars
The Magnitude Scale
First introduced by Hipparchus (160 - 127 B.C.):
• Brightest stars: ~1st magnitude
• Faintest stars (unaided eye): 6th magnitude
More quantitative:
• 1st mag. stars appear 100 times brighter than 6 th mag. stars
• 1 mag. difference gives a factor of 2.512 in apparent brightness (larger magnitude => fainter object!)
Betelgeuse
Rigel
Magnitude = 0.41 mag
Magnitude = 0.14 mag
The Magnitude Scale (Example)
For a magnitude difference of 0.41 – 0.14 = 0.27, we find an intensity ratio of (2.512)0.27 =
1.28.
In other words, Rigel is 1.28 times brighter than Betelgeuse.
The Magnitude Scale (2)
Sirius (brightest star in the night sky): mv = -1.42Full moon: mv = -12.5
Sun: mv = -26.5
The magnitude scale system can be extended towards negative numbers (very bright) and
numbers greater than 6 (faint objects):
The Celestial Sphere
Celestial equator =
projection of Earth’s
equator onto the c.s.
Zenith = Point on the celestial sphere directly overhead
Nadir = Point on the c.s. directly underneath (not visible!)
North celestial pole = projection of
Earth’s north pole
onto the c.s.
Distances on the Celestial SphereThe distance between two stars on the celestial
sphere can only be given as the difference between the directions in which we see the stars.
Therefore, distances on the celestial sphere
are measured as angles, i.e., in
degrees (o):
Full circle = 360o
arc minutes (‘):
1o = 60’
arc seconds (“):
1’ = 60”
The Celestial Sphere (2)• From geographic latitude l (northern hemisphere), you see the
celestial north pole l degrees above the northern horizon;
l
90o - l
• Celestial equator culminates 90º – l above the horizon
• From geographic latitude –l (southern hemisphere), you see the celestial south pole l degrees above the southern horizon
The Celestial Sphere (Example)
The Celestial South Pole is not visible from the northern hemisphere.
Horizon
North
Celestial North Pole
40.70
South
49.30
Celestial Equator
Horizon
New York City: l ≈ 40.7º
The Celestial Sphere (3)
Apparent Motion of The Celestial Sphere
Looking north, you will see stars apparently circling counterclockwise around the Celestial North Pole.
Apparent Motion of The Celestial Sphere (2)
Some constellations
around the Celestial North Pole never set.
These are called “circumpolar”.
The circle on the celestial sphere containing the circumpolar constellations is called the
“circumpolar circle”.
Apparent Motion of The Celestial Sphere (3)
Looking east, you see stars
rising and moving to the
upper right (south)
Looking south, you see stars moving to the right (west)
Precession (1)
The Sun’s gravity is doing the same to Earth.
The resulting “wobbling” of Earth’s axis of rotation around the vertical w.r.t. the Ecliptic takes about 26,000 years and is
called precession.
At left, gravity is pulling on a slanted top. => Wobbling around the vertical.
Precession (2)As a result of precession, the celestial north
pole follows a circular pattern on the sky, once every 26,000 years.
It will be closest to Polaris ~ A.D. 2100.
There is nothing peculiar about Polaris
at all (neither particularly bright nor
nearby etc.)
~ 12,000 years from now, the celestial north pole will be
close to Vega in the constellation Lyra.
The Sun and Its Motions
Earth’s rotation is causing the day/night cycle
The Sun and Its Motions (2)
The Sun’s apparent path on the sky is called the Ecliptic.
Equivalent: The Ecliptic is the projection of Earth’s orbit onto the celestial sphere.
Due to Earth’s revolution around the sun, the sun appears to move through the zodiacal
constellations.
The Seasons
Earth’s axis of rotation is inclined vs. the normal to its orbital plane by 23.5°, which causes the seasons.
The Seasons (2)The Seasons are caused only by a varying
angle of incidence of the sun’s rays.
We receive more energy from the sun when it is shining onto the Earth’s surface under a
steeper angle of incidence.
The Seasons (3)
The seasons are not related to Earth’s distance from the sun. In fact, Earth is slightly closer to the sun in
(northern-hemisphere) winter than in summer.
Light from the sun
Steep incidence → Summer
Shallow incidence → Winter
The Seasons (4)
Northern summer = southern winter
Northern winter = southern summer
The Seasons (5)
Earth’s distance from the sun has only a very minor influence on seasonal
temperature variations.
Sun
Earth in July
Earth in January
Earth’s orbit (eccentricity greatly exaggerated)
The Motion of the Planets
The planets are orbiting the sun almost exactly in the plane of the Ecliptic.
Jupiter
Mars Earth
Venus
Mercury
Saturn
The Moon is orbiting Earth in almost the same plane (Ecliptic).
The Motion of the Planets (3)
Mercury appears at most ~28° from the sun.
It can occasionally be seen shortly after sunset in the west or before sunrise in the east.
Venus appears at most ~46° from the sun.
It can occasionally be seen for at most a few hours after sunset in the west or before sunrise in the east.
Astronomical Influences on Earth’s Climate
Factors affecting Earth’s climate:
• Eccentricity of Earth’s orbit around the Sun (varies over period of ~ 100,000 years)
• Precession (Period of ~ 26,000 years)
• Inclination of Earth’s axis versus orbital plane
Milankovitch Hypothesis: Changes in all three of these aspects are responsible for
long-term global climate changes (ice ages).
Astronomical Influences on Earth’s Climate (2)
Last glaciation
End of last glaciation
Polar regions receive more than average energy from the sun
Polar regions receive
less than average energy
from the sun