# The conversion from solar mass to g is done in the orbital params function since dsep tracks
# everyging in either solar units or log solar uints
a = orbital_params(basedMDwarfModel.mass, 0.075, period)

dt = (times[1] - times[0]) * 60

BrownDwarfTemps = list()
bdtemp = BDTEMP
bdmass = 0.075 * SMASS

# Here is a handwavey thing. I am basically assuming that all the energy
#  dumped onto the star stays in the atmosphere (and that the atmosphre is 
#  and idea monatomic gas (f=3))
N = estimateParticlesBBN(bdmass*BDATMMFRAC)

# this is used to figure out how much energy the star radiates away so
#  that some interneral energy fudge factor can be added to keep the
#  atmosphere from rapidly cooling to 0
initialCooling = bdtemp - cool_blackbody(BDRAD, bdtemp, bdmass, dt, 0)

# Due to the high temporal resolutions required to resolve flares and the long
# baseline needed to heat the star I run this section to just fine the mean 
# temperature change per orbit.
porbitID = 0
temps = list()
pOrbitTemp = bdtemp
for tid, (t, l) in enumerate(zip(times, hemiLuminosity)):
    orbitID = t // period
    if orbitID != porbitID:
        temps.append(bdtemp - pOrbitTemp)
        pOrbitTemp = bdtemp
        porbitID = orbitID
    incidentUponBD = incident_luminosity(l, sphere.radius, 1.001e+10, a)
    bdtemp = calculate_new_surface_params(incidentUponBD, bdtemp, bdmass, dt)
    BrownDwarfTemps.append(bdtemp)