1) How massive would Earth had been if it had accreted hydrogen compounds in addition to the sme properties listed in table 7.1? (Assume the same properties of the ingredients as listed in the table) 2) Now imagine that Earth had been able to capture hydrogen and helium gas in the same proportions as listed in the table. How massive would it have been?
1) How massive would Earth had been if it had accreted hydrogen compounds in addition to the sme properties listed in table 7.1? (Assume the same properties of the ingredients as listed in the table) 2) Now imagine that Earth had been able to capture hydrogen and helium gas in the same proportions as listed in the table. How massive would it have been?
1) How massive would Earth had been if it had accreted hydrogen compounds in addition to the sme properties listed in table 7.1? (Assume the same properties of the ingredients as listed in the table) 2) Now imagine that Earth had been able to capture hydrogen and helium gas in the same proportions as listed in the table. How massive would it have been?
1) How massive would Earth had been if it had accreted hydrogen compounds in addition to the sme properties listed in table 7.1? (Assume the same properties of the ingredients as listed in the table)
2) Now imagine that Earth had been able to capture hydrogen and helium gas in the same proportions as listed in the table. How massive would it have been?
Transcribed Image Text:TABLE 7.1 The Planetary Data
Average
Distance
Average
Equatorial
Radius (km) (Earth = 1) (g/cm³) Period
Relative
Average
Surface (or
Cloud-Top)
Temperature
Photo
Planet
from Sun
Size
(AU)
Mass
Known
Orbital
Rotation
Axis
Мoons
Period
Tilt
Composition
(2018)
Rings?
Mercury
0.387
2440
87.9
700 K (day)
100 K (night)
0.055
No
58.6 days
0.0°
Rocks, metals
days
Venus
0.723
6051
0.82
5.24
Rocks, metals
No
243 days
177.3°
740 K
Earth
1.00
6378
23.93
Rocks, metals
No
1.00
23.5°
290 K
hours
Мars
2
No
1.52
3397
24.6
220 K
Rocks, metals
0.11
25.2°
hours
H, He, hydrogen
compoundsº
Jupiter
79
Yes
5.20
71,492
318
9.93
3.1°
125 K
1.33
hours
H, He, hydrogen
62
Yes
Saturn
9.54
10.6
26.7°
95 K
compounds
60,268
95.2
0.70
hours
H, He, hydrogen
compoundsº
Uranus
17.2
97.9°
60 K
27
Yes
19.2
25,559
14.5
1.32
hours
H, He, hydrogen
compounds
165
16.1
Neptune
30.1
24,764
17.1
1.64
29.6°
60 K
14
Yes
years
hours
Pluto
39.5
248
6.39 days
1185
0.0022
1.9
112.5°
44 K
Ices, rock
No
years
Eris
67.7
1168
0.0028
2.3
557
1.08 days
78°
43 K
Ices, rock
years
1
No
Including the dwarf planets Pluto and Eris; Appendix E gives a more complete list of planetary properties
Surface temperatures for all objects except Jupiter, Saturn, Uranus, and Neptune, for which cloud-top temperatures are listed
Includes water (H,0), methane (CH4), and ammonia (NH3)
vidually, the comparative planetology approach has der
onstrated its value in at least three key ways:
(continued from page 191)
While we still can learn much by studying planets inc
- Comparative study has revealed similarities and differ
ences among the planets that have helped guide th
development of our theory of solar system formation
thereby giving us a better understanding of how we
came to exist here on Earth.
- Comparative study has given us new insights into the
physical processes that have shaped Earth and other
worlds-insights that can help us better understand and
manage our own planet.
• Comparative study has allowed us to apply lessons from
our solar system to the study of the many planetary sys-
tems now known around other stars. These lessons help
us understand both the general principles that govern
planetary systems and the specific circumstances under
which Earth-like planets-and possibly life-might
The comparative planetology approach should also
benefit you as a student by helping you stay focused on
processes rather than on a collection of facts. We now know
so many individual facts about the worlds of our solar
system and others that even planetary scientists have trouble
keeping track of them all. By concentrating on the processes
that shape planets, you'll gain a deeper understanding of
how planets, including Earth, actually work.
exist elsewhere.
等|三
7.2 Patterns in the Solar System
One of our major goals in studying the solar system as a
whole is to understand how it formed. In this section, we’ll
explore key patterns that must be explained by a theory of
solar system formation.
te
Four Features of the Solar System
ea
What features of our solar system provide
clues to how it formed?
Fea
sho
the
sent
T
are t
Venu
and a
one of the numbered steps in Figure
1. Patterns of motion ar
planets, and larg
very organi
2. T
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