mercury surface erosion and sun-induced exospheric escape
DESCRIPTION
Mercury surface erosion and sun-induced exospheric escape Stefano Orsini, Anna Milillo, Alessandro Mura @INAF-IFSI, Roma, Italy. Mercury has an extremely thin mantle/crust, so that it is the densest terrestrial planet in the solar system. - PowerPoint PPT PresentationTRANSCRIPT
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Mercury has an extremely thin mantle/crust, so that it is the densest terrestrial planet in the solar system.
May sun-induced loss processes be considered as responsible for Mercury surface erosion?
Not proved, but… this is a fascinating hypothesis, which needs observations
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OUTLINE• In this presentation, we approach the Hermean surface
evolution task by applying the Environment SimulationTool (EST) developed by Mura et al (2007), able to derive the exospheric profiles (both gravitationally bound and escaping), depending on external input parameters (surface composition, solar and space conditions, etc.).
• In view of a more refined calculation, we now simply apply EST to the O component by using two different solar conditions: the present one, and the one expected at the solar system formation, about 4.5 Gy ago.
• No other assumptions, (e.g.: related to the possible different evolving planet characteristics) have been presently considered, but they will be added in the future.
OUTLINE
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Evolution of the Solar Radiation and of the Solar Wind
[Newkirk, Jr.: Geochi. Cosmochi. Acta Suppl., 13, 293301; Kulikov et al.: PSS, 54, 1325, 2006]
Total Luminosity Energetic Radiation
Solar Wind Velocity
[Guinan and Ribas: ASP, 269, 85 – 107, 2002]
[Ribas et al.: ApJ, 622, 680 – 694, 2005]
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EST application: escape rate estimateINPUT DATAASSUMPTIONS
• (Young Sun) UV Radiation: Actual * 100 Luminosity Actual – 30% SW vel Actual * 4 SW dens Actual * 100• (Exosphere) Ionisation lifetime Actual / 100• (Soil) Soil density 2 g/cm^3 Oxygen abundance 50% Binding Energy 3 eV Only 3 processes considered: PSD, IS, TD
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EST: PSD and IS exospheric refilling. Profiles vs, some external solar
parameters
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Mercury exospheric profiles: solar conditions: today
Ion SputteringPhoton-stimulated Desorption
Thermal Desorption,
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Mercury O Exospheric Loss rates: Solar Conditions: today
RM= 2440 km = 2440000 m SM= 4*pi* RM2 = 7.481E13 m2
ds= 2 g/cm3 = 2000 kg/m3 Gy=3.157E+16 s
Erosion = Er (m/Gy)= rate/(SM* ds)*1Gy = rate * 0.211
IS + PSD + TD Rate (part/s) Rate (Kg/s)Jeans Escape 0.45165E+27 0.11996E+02
Photoionisation 0.78408E+26 0.20825E+01Total 5.3E+26 14(Er=3m/Gy)
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Mercury O Exospheric Profiles: Solar Conditions: 4,5 Gy ago
Thermal Desorption
Photon-stimulated DesorptionIon Sputtering
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Mercury Surface O Particle EscapeSolar Conditions:
TODAY
Mercury Surface O Particle EscapeSolar Conditions:
4,5 Gy Ago
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IS Rate (part/s) Rate (Kg/s)Jeans Escape 0.34292E+30 0.12606E+04
Photoionisation 0.26528E+29 0.94205E+03total 3.7E+29 2200PSD
Jeans Escape 0.45979E+28 0.12212E+03Photoionisation 0.16460E+31 0.43717E+05
total 1.6E+30 43840TD
Jeans Escape 0.58323E+13 0.15491E-12Photoionisation 0.76708E+23 0.20374E-02
total 7°.7+23 0.0002
Total 2.0E+30 46040(Er=10km/Gy)
Mercury Exospheric O Loss rates: Solar Conditions: 4,5 Gy ago
RM= 2440 km = 2440000 m SM= 4*pi* RM2 = 7.481E13 m2
ds= 2 g/cm3 = 2000 kg/m3 Gy=3.157E+16 s
Erosion = Er (m/Gy)= rate/(SM* ds)*1Gy = rate * 0.211
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CONCLUSIONS
• We have applied the EST code developed by Mura et al (2007), to derive the escaping O intensity using two different solar conditions: the present one, and the one expected at the solar system formation, about 4.5 Gy ago.
• Significant differences have been noticed, so that the mass amount eroded by the young sun is quite significant (about 10 km/Gy); whereas at present the erosion rate is of the order of a few meters/Gy
• These calculations encourage to further refine our approach, in order to get a more reliable result
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MANY THANKSFOR YOUR ATTENTION!
SPECULATIONS?SO MANY.....