The Solar System I - Planets Flashcards
differences between terrestrial and jovian planets what aspecs make it suitable to have an atmosphere rings jupitars atmosphere uranus special orientation
Terrestrial Planets:
Distance from the sun:
size:
composition:
density:
1)less than 2 AU
2)small
3)iron, oxygen, silicon, madneisum, nickel, sulfur
4)high
Jovian Planets:
Distance from the sun:
size:
composition:
density
1_More than 5AU
2)Large
3)Light elements: hydrogen, helium
4)Low
Planetry ring formation:
if satellite is outside –1— limit, tidal forces may deform satellite but will not —2— it apart
is satellite is inside Roche limit, tidal forces overwhelm —3—- forces that hold satellite togther and satellite —-4— apart.
Closer fragments orbit —5— —> spreads fragments around planet
1) roche
2) tear
3) gravitational
4) fragments
5) faster
Jupiter shows several
distinctive features
* Presence of —1—- on
its poles
* Most common ones:
* Great —2— Spot
* Belts (dark/red-ish
areas)
* Zones (light/grey-ish
areas)
1)aurorae
2)Red
Great red spot known for over a century
* Jupiter’s atmosphere does not seem to suffer significant changes over
the years»_space;> —1—-!!!
* New features are constantly appearing and disappearing from Jupiter’s atmosphere.
* Some of them even observable with amateur —2—–
1)False
2)telescope
The Great red spot takes –1— days to complete one rotation
* It –2— changes with time, ranging from 40,000 km (~3xEarth’s size) to just 14,000 km (~Earth’s size).
* Currently —3— to new minima
* Results from 2015 show that the shrinking rate is slowing down
1) six
2) size
3)shrinking
No clear features are easily seen on Uranus
* Its axis of —1— is fully tilted with the –2— plane –3— to the —4— plane
1)rotation
2)orbital
3)perpendicular
4)equatorial
—1—, —2— and —-3— information can be used to see some features on uranus’ atmosphere
features are not easily seen because they formed in the —4—-
upper atmosphere = 82% —-5—-, 15%—-6—-, 2% —7— ( absorbs light of the —6– end of the spectrum)
1)infrared
2)ultraviolet
3)optical
4)troposphere
5)hyrdogen
6)helium
7)methane
8)red
Detection metods for expoplanets
Radial velocity method:
A star has characteristic 1? lines, depending on its 2? type (cf. lab expt.)
* If a star is 3?, we detect
spectral lines at their laboratory
wavelengths (λ)
* If a star has 3? (planet
or star) then the λ’s of the star’s
spectral lines get Doppler shifted
since the star now has 4?
relative to the centre of mass of
the solar system
1) spectral
2) spectral
3) alone
4) companions
5) motion
Radial velocity method
Only –1— mass is determined with this method, since we can’t determine inclination of –2— plane to our line of sight
1)minimum
2)orbital
1) planet transits to —1— of star»_space; blocks part of star’s visible light»_space; amount of —2— tells us about diameter
2) when planet moves —3— front of star the 4? features in the star’s spectrum reveals the 5? of the planet’s atmosphere
3) amount of 6? dimming when planet moves 7? star tells about 8? 9?
2)1)front
2)diameter
3)from
4)absorption
5)composition
6)infrared
7)behind
8)surface
9)temperature
Habitable Zone
1? from a star at which liquid water can exist on the planets surface. Neither too hot or too cold. A star’s habitable zone is different depending on the star’s sizes and 2?.
1)distance
2)brightness
Rocky objects ranging between few 1? up to 1000km in 2?
Most of them are 3? between the orbits of 4? and 5?
1)kilometres
2)diameter
3)located
4)Mars
5)Jupiter
Some astreroids are so low in 1? that they cannot be made of solid 2? They are made of small fragments joined together due to 3?
1)meteoroid = small object moving across solar system
2)meteor = flash of light as meteroid enters earth’s atmosphere. meteroids star burning at 50km
when meteoroid enters earth’s atmosphere, the air in front of it heats up to 3000K - producing a bright tail
3)meteorite is a piece of rock that has survives the descent through Earth’s atmosphere and has reached the ground
