Planetary Fluxes
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User provides IR and Vis tables, which are fit with sin functions, whose parameters are fed to KRC ([[File:67.1_AvgFluxes.txt]]). | User provides IR and Vis tables, which are fit with sin functions, whose parameters are fed to KRC ([[File:67.1_AvgFluxes.txt]]). | ||
| − | [[Image:Phobos_Fluxes_2.png]] | + | [[Image:Phobos_Fluxes_2.png|600px]] |
PLOT FITS | PLOT FITS | ||
Revision as of 12:29, 22 January 2019
Incoming visible and IR fluxes contributed by nearby bodies can be specified, for example Mars shine on Phobos, or Jupiter shine on Europa. Set:
PFlux = "T" Lon_Hr = [0-24]
in KRC, fluxes take the form of sin functions characterized by various nonintuitive parameters (see helplist).
The DaVinci interface generates these parameters and feed them to KRC from default parameters or user-defined values. In both cases, various assumptions and fits are performed.
While the incoming visible flux is generally straightforward to calculate, the incoming IR flux can be more complex to determine for bodies with strong diurnal temperature variations (like Mars, unlike Jupiter for example).
Fixed Diurnal Temperatures (Jupiter, Saturn, Uranus, Neptune, etc.)
This case applies to satellites revolving around gas giants, or low diurnal contrast bodies (Venus, if it had satellites) etc. The IR flux is only a function of the solid angle of the emitting body. The visible flux follows a sin function over the course of a day. Fewest assumptions used.
The simplest approach consist in using default builtin values from the KRC support files:
OUT = krc(lat = 0., INERTIA = 70., body = "Jupiter,Europa", bodytype = "minor", ALBEDO = 0.55, PFlux = "T", Lon_Hr = 12., LKofT = "F")
But any input value can be forced:
- BT_Avg : Average Brightness Temperature [K]
- BT_Min : Min Brightness Temperature, if diurnal cycle [K]
- BT_Max : Max Brightness Temperature [K]
- Dis_AU : Distance from Sun in AU
- Geom_alb : Geometric Albedo [1]
- Mut_Period : Mutual Period [?]
- Orb_Radius : Orbiting Radius [km]
- Radius : Radius of the Orbiting body [km]
- Lon_Hr : Longitude Hour of the surface point (see above)
OUT = krc(lat = 0., INERTIA = 70., body = "Jupiter,Europa", bodytype = "minor", ALBEDO = 0.55, PFlux = "T", BT_Avg = 127., BT_Min = 127., BT_Max = 127., Dis_AU = 5.203, Geom_alb = 0.52, Mut_Period = 3.55, Orb_Radius = 670900, Radius = 670900, Lon_Hr = 12., LKofT = "F")
Noticeable Diurnal Temperatures Cycle (Mars, Pluto, etc.)
This case applies to satellites revolving around planets experienced pronounced diurnal cycles like Phobos around Mars. The IR flux is not only a function of the solid angle of the emitting body, but also a function of the local time of the emitting body.
- IR and Vis Tables
User provides IR and Vis tables, which are fit with sin functions, whose parameters are fed to KRC (File:67.1 AvgFluxes.txt).
PLOT FITS
PLOT WITH and WITHOUT FLUXEs
- The IR and visible fluxes are modeled by fitting a sin wave through the max and min radiance values, and KRC accepts parameters describing these two sin functions (IR, and VIS).
- The IR and visible fluxes are derived elsewhere, and fit with a sin function.
Buffer = ascii("~/Google Drive/THEMIS_PHOBOS/09_29_2017/67.1_AvgFluxes.txt",format=float)
Vis = cat(Buffer[3,,1]+00,(Buffer[1,,1]+00.)%24.,axis=x) #Potential Bug with the IR flux? => Check this
IR = cat(Buffer[2,,1]+65,(Buffer[1,,1]+00.)%24,axis=x)
Lon_Hr = 12.
test = krc_planetary_flux_table(IR,Vis,Lon_Hr)
test_T = krc(INERTIA=35.,lat=10.,lon=0.,body="Mars,Phobos",bodytype="minor",ls=Ls,PFlux="T",Lon_Hr=Lon_Hr,IR=IR,Vis=Vis,ALBEDO=Alb,EMISS=EMIS)
Time = (test_T.time + 12.) % 24.
plot(test_T.tsurf[,1,1],xaxis=Time)
EXAMPLE HERE. PLOT Fluxes from outside MODEL INCLUDING FIT TO OUTSIDE MODEL
Davinci function krc_planetary_flux_table(IR,Vis,Lon_Hr) DaVinci function krc_planetary_flux_porb(porb,porb_Planet,Lon_Hr)
