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6. STARS
Stars are massive, luminous
sphere of hot gas cloud, held
together by gravity, main element
is Hydrogen. Stars
Properties of
    1. generate energy by itself
    2. Have an evolution to build a
  massive element such as Helium
  , Lithium and Beryllium
      The nearest star to Solar
    system is Alpha Centauri
Star-forming region in Orion’s
Belt
newly-formed star
clusters
Cloud Collapse - occurs deep in cloud
“Pillars of Creation”




Visible light - Hubble        Near Infrared light
Space Telescope (HST)         - ESO Very Large
                              Telescope (VLT)
“EGGS” (Evaporating Gaseous Globules)




Dense regions forming new stars -
surrounding gas & dust “eaten into”
by strong stellar winds, UV photons
& ionization fronts
QuickTime™ an d a
                          Sorenson Video deco mpressor
                          are need ed to see this p icture .




IR (infrared) sees
deeper than visible
light & detects thermal
emission of warm dust
Dark clouds &
deeply embedded
young stars with
gas outflows and
Herbig-Haro (HH)
objects
Some
young
disks & jets
revealed
“proplyds”
(protoplanetary disks)
seen in star-forming
regions
6.1 Stars Evolution
  The formation of a star begins
with gravitational instability within
the nebula.
  When the hot cloud has
approximately reached the stable
condition of hydrostatic
equilibrium, a Protostar.
• Low mass stars , not much light ,
  use less fuel , have a long life and
  end up not a bomb.

• Massive stars that are very light
  and fuel consumption rate is very
  high. Will have a short life span.
  And ending with a violent
  explosion called a supernova.
Mass of protostar (M) Star Evolution
comcompare with Mass
   of the Sun M
M ≥ 25 M               Blue giant star
                       Final : Black
                       Hole
9M ≤ M ≤ 25M           Blue giant star
                       Red giant star
                       Final : Neutron
                       Star
Conclusio
   n:
  Super massive
  Stars
   Blue giant star

     Supernova
      Black hole
      Nebula
Massive Stars

 Red Giant Star

   Supernova
    Neutron Star +
    Nebula
Small star


  Red giant star
   white Dwarf
    planetary
   nebula
6.2 Birth and
evolution of the Sun
G2
5,000              10,000


             100



                      1
100
6.3 Brightness and
     Magnitude
 Brightness
                      1




Magnitude
1
      2.512
      5                      2.512   5

100

       -26.7
                     -4.5
                      -0.5
              0.45
                     1.2
Apparent magnitude
         describes the relative
brightness of objects as they appears
in sky from the Earth.
   Absolute magnitude
          the apparent magnitude it
would have if it were at a distance of
10 parsecs (32.6 light-years) from
Earth.
6.4 Color and
Temperature
Color of the star related to
surface temperature
    , is divided in 7 Spectral
type.
   And related to lifetime of
stars. (                   ) that
the youngest stars is Blue , the
oldest stars is Red.
O             O 9.5
    30,000
B   30,000-    B3
    10,000

A   10,000-    A2
    7,500
F   7,500-     F5
    6,000
6.5 Determination
    of Distance
         Parallax)




                     2
•


• Parsec”      Parallax Angle of 1
  Arc Second
          AU
•
•

               r = 1/p

    r=               distance)
         pc)
    p=           parallax angle)
Regulus)


     r = 1/p
       = 1/(0.04)

                    x 3.26 = 81.5

            x 206,265 = …………….
AU
6.6 Nebula
1.
         Great Nebula)
•
                M42
2.
•


•

         IC 434
3.
•


•        Charles Messier




         M1
4.
•
         Monoceros)

•             NGC 2237
5.
     Trifid Nebula)
•
The Pleiades
6.7 Stellar system
  1. Binary star systems: two stars are
 gravitationally bounded and they
 orbit each other ex. Sirius , Procyon
 2. Triple star systems : Alpha
 Centauri A,B,C
 3. Star cluster ex. The Pleiades ,
 Great Globular Cluster in Hercules
 M13.
6.8 Mass of
 the Stars
• Mass is the matter of the Star
• Tiny Star have low gravitational
  force, low pressure of hot gas,
  useless fuel.
• Measuring the mass of distant
  stars is Newton’s version of
  Kepler’s Third Law of orbital
  motion because motion period

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Lesson 6 stars

  • 2. Stars are massive, luminous sphere of hot gas cloud, held together by gravity, main element is Hydrogen. Stars Properties of 1. generate energy by itself 2. Have an evolution to build a massive element such as Helium , Lithium and Beryllium The nearest star to Solar system is Alpha Centauri
  • 3. Star-forming region in Orion’s Belt
  • 5. Cloud Collapse - occurs deep in cloud
  • 6. “Pillars of Creation” Visible light - Hubble Near Infrared light Space Telescope (HST) - ESO Very Large Telescope (VLT)
  • 7. “EGGS” (Evaporating Gaseous Globules) Dense regions forming new stars - surrounding gas & dust “eaten into” by strong stellar winds, UV photons & ionization fronts
  • 8. QuickTime™ an d a Sorenson Video deco mpressor are need ed to see this p icture . IR (infrared) sees deeper than visible light & detects thermal emission of warm dust
  • 9.
  • 10.
  • 11. Dark clouds & deeply embedded young stars with gas outflows and Herbig-Haro (HH) objects
  • 14. 6.1 Stars Evolution The formation of a star begins with gravitational instability within the nebula. When the hot cloud has approximately reached the stable condition of hydrostatic equilibrium, a Protostar.
  • 15. • Low mass stars , not much light , use less fuel , have a long life and end up not a bomb. • Massive stars that are very light and fuel consumption rate is very high. Will have a short life span. And ending with a violent explosion called a supernova.
  • 16. Mass of protostar (M) Star Evolution comcompare with Mass of the Sun M M ≥ 25 M Blue giant star Final : Black Hole 9M ≤ M ≤ 25M Blue giant star Red giant star Final : Neutron Star
  • 17.
  • 18. Conclusio n: Super massive Stars Blue giant star Supernova Black hole Nebula
  • 19. Massive Stars Red Giant Star Supernova Neutron Star + Nebula
  • 20. Small star Red giant star white Dwarf planetary nebula
  • 22. G2 5,000 10,000 100 1 100
  • 23.
  • 24. 6.3 Brightness and Magnitude Brightness 1 Magnitude
  • 25. 1 2.512 5 2.512 5 100 -26.7 -4.5 -0.5 0.45 1.2
  • 26. Apparent magnitude describes the relative brightness of objects as they appears in sky from the Earth. Absolute magnitude the apparent magnitude it would have if it were at a distance of 10 parsecs (32.6 light-years) from Earth.
  • 28. Color of the star related to surface temperature , is divided in 7 Spectral type. And related to lifetime of stars. ( ) that the youngest stars is Blue , the oldest stars is Red.
  • 29.
  • 30. O O 9.5 30,000 B 30,000- B3 10,000 A 10,000- A2 7,500 F 7,500- F5 6,000
  • 31. 6.5 Determination of Distance Parallax) 2
  • 32. • • Parsec” Parallax Angle of 1 Arc Second AU •
  • 33.
  • 34. r = 1/p r= distance) pc) p= parallax angle)
  • 35. Regulus) r = 1/p = 1/(0.04) x 3.26 = 81.5 x 206,265 = ……………. AU
  • 37. 1. Great Nebula) • M42
  • 38.
  • 39. 2. • • IC 434
  • 40.
  • 41. 3. • • Charles Messier M1
  • 42.
  • 43. 4. • Monoceros) • NGC 2237
  • 44.
  • 45. 5. Trifid Nebula) •
  • 46.
  • 48. 6.7 Stellar system 1. Binary star systems: two stars are gravitationally bounded and they orbit each other ex. Sirius , Procyon 2. Triple star systems : Alpha Centauri A,B,C 3. Star cluster ex. The Pleiades , Great Globular Cluster in Hercules M13.
  • 49. 6.8 Mass of the Stars • Mass is the matter of the Star • Tiny Star have low gravitational force, low pressure of hot gas, useless fuel. • Measuring the mass of distant stars is Newton’s version of Kepler’s Third Law of orbital motion because motion period