1) How massive would Earth had been if it had accreted hydrogen compounds in addition to the rock and metal 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 addition to the rock and metal properties, in the same proportions as listed in the table. How massive would it have been? TABLE 7.1 The Planetary DataAverageDistanceAverageEquatorialRadius (km) (Earth = 1) (g/cm³) PeriodRelativeAverageSurface (orCloud-Top)TemperaturePhotoPlanetfrom SunSize(AU)MassKnownOrbitalRotationAxisМoonsPeriodTiltComposition(2018)Rings?Mercury0.387244087.9700 K (day)100 K (night)0.055No58.6 days0.0°Rocks, metalsdaysVenus0.72360510.825.24Rocks, metalsNo243 days177.3°740 KEarth1.00637823.93Rocks, metalsNo1.0023.5°290 KhoursМars2No1.52339724.6220 KRocks, metals0.1125.2°hoursH, He, hydrogencompoundsºJupiter79Yes5.2071,4923189.933.1°125 K1.33hoursH, He, hydrogen62YesSaturn9.5410.626.7°95 Kcompounds60,26895.20.70hoursH, He, hydrogencompoundsºUranus17.297.9°60 K27Yes19.225,55914.51.32hoursH, He, hydrogencompounds16516.1Neptune30.124,76417.11.6429.6°60 K14YesyearshoursPluto39.52486.39 days11850.00221.9112.5°44 KIces, rockNoyearsEris67.711680.00282.35571.08 days78°43 KIces, rockyears1NoIncluding the dwarf planets Pluto and Eris; Appendix E gives a more complete list of planetary propertiesSurface temperatures for all objects except Jupiter, Saturn, Uranus, and Neptune, for which cloud-top temperatures are listedIncludes water (H,0), methane (CH4), and ammonia (NH3)vidually, the comparative planetology approach has deronstrated 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 differences among the planets that have helped guide thdevelopment of our theory of solar system formationthereby giving us a better understanding of how wecame to exist here on Earth.- Comparative study has given us new insights into thephysical processes that have shaped Earth and otherworlds-insights that can help us better understand andmanage our own planet.• Comparative study has allowed us to apply lessons fromour solar system to the study of the many planetary sys-tems now known around other stars. These lessons helpus understand both the general principles that governplanetary systems and the specific circumstances underwhich Earth-like planets-and possibly life-mightThe comparative planetology approach should alsobenefit you as a student by helping you stay focused onprocesses rather than on a collection of facts. We now knowso many individual facts about the worlds of our solarsystem and others that even planetary scientists have troublekeeping track of them all. By concentrating on the processesthat shape planets, you'll gain a deeper understanding ofhow planets, including Earth, actually work.exist elsewhere.等|三7.2 Patterns in the Solar SystemOne of our major goals in studying the solar system as awhole is to understand how it formed. In this section, we’llexplore key patterns that must be explained by a theory ofsolar system formation.teFour Features of the Solar SystemeaWhat features of our solar system provideclues to how it formed?FeashothesentTare tVenuand aone of the numbered steps in Figure1. Patterns of motion arplanets, and largvery organi2. T

How massive would Earth had been if it had accreted hydrogen compounds in addition to the rock and metal properties listed in table 7.1? Shock-induced devolatilization of the accreting materials happens when a protoplanet grows with increasing accretional energy, and volatile species are moved into the developing atmosphere, limiting the quantity of volatiles that can be buried within a planet. When the planetesimal mass approaches that of Mars, Ahrens et al. (1989) found that efficient loss of CO2 and H2O from accreting solids on impact occurs. Above this size, degassing would be aided by substantial melting caused by accretional energy deposition, as well as a radiative blanketing effect if a water-rich atmosphere had formed or a thick atmosphere had been gravitationally displaced.

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Applications and Investigations in Earth Science (9th Edition)

9th Edition

ISBN:9780134746241

Author:Edward J. Tarbuck, Frederick K. Lutgens, Dennis G. Tasa

Publisher:Edward J. Tarbuck, Frederick K. Lutgens, Dennis G. Tasa

Chapter1: The Study Of Minerals

Section: Chapter Questions

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1) How massive would Earth had been if it had accreted hydrogen compounds in addition to the rock and metal 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 addition to the rock and metal properties, in the same proportions as listed in the table. How massive would it have been?