<jupyter_start><jupyter_text>Asteroid Family Package -- Functions:- asteroid_family.homogeneus_family: create a homogeneus asteroid family- asteroid_family.differentiated_family: create a homogeneus asteroid family- asteroid_family.mass_distribution: create a mass distribution normalized by the total mass- asteroid_family.min_Vej: minimum ejection velocity- asteroid_family.mean_vej: maximum ejection velocity- asteroid_family.mean_vej_distribution: - asteroid_family.velocity_field- asteroid_family.catastrophic_energy: obtain the catactrophic energy based on a model from Stewart and Leinhardt(2009).- asteroid_family.yarkovsky_dadt: obntain the semi-axis varition in time from the Yarksovskt Effect in function of the physical parameters of the asteroid- asteroid_family.yakovsky_change_unit: function to change the units of dat/dt from asteroid_family.yarkovsky_dadt- asteroid_family.mag_absoluta: obtain the absolute magnitude, H, for a set of asteroids, given a geometric albedo and diameter. Based on Parker et al.(2008).  Including information for the parental body }and its location on asteroid min belt<jupyter_code>#Parental data
rpb = 20 #km

rho_mantle = 3.
rho_core = 7.

pv_mantle = 0.4
pv_core = 0.15

Vi = 5 #km/s impact velocity
fke = 0.01 #inelastic
#location in the Main Belt --> same as 298 Baptistina
M       = 280.1642437983165 #degrees
peri    = 135.1543076468920 #degrees
node    = 8.253490030039535 #degrees
i       = 6.28752726137564 #degrees
e       = 0.09612545504215386
a       = 2.26362004764974 #AU
period  = 3.41 #year
ano     = 2013
mes     = 11
dia     = 4
da0     = 0<jupyter_output><empty_output><jupyter_text>Creating the synthetic differentiated asteroid family<jupyter_code>help(asteroid_family.differentiated_family)
mass, vej, rho, radius, mag = asteroid_family.differentiated_family('H',rpb,rho_mantle,rho_core,
                                                          Vi,fke,0.5,pv_core,pv_mantle,'YES')<jupyter_output>Obtain velocity field: duration [seconds] = 0.22031927108764648<jupyter_text>Obtain the Initial velocity field<jupyter_code>VT, VR, VW, A, E, I, dA, dE, dI = asteroid_family.gauss_equations(vej, a, e, i, period, 'YES')<jupyter_output>Applied Gauss Equations: duration [seconds] = 0.026523590087890625<jupyter_text>Obtain the semi-axis variation in time from the Yarkovsky effect<jupyter_code>dadt = asteroid_family.yarkovsky_dadt(2*radius,np.random.uniform(0,np.pi,len(mass))*180./np.pi)<jupyter_output><empty_output><jupyter_text>Saving in a dataframe and .csv file using Pandas Package<jupyter_code>data = pd.DataFrame([massa, vej, rho, raio, mag,VT, VR, VW, A, E, I, dA, dE, dI, dadt]).T
data.columns = ['mass', 'vej', 'density', 'radius', 'H', 'VT', 
                'VR', 'VW', 'A', 'E', 'I', 'dA', 'dE', 'dI', 'dadt']
data
plt.figure(figsize=(9,6))
#plt.grid(color='white')
plt.scatter(data.radius[data.density == 3],data.dadt[data.density == 3], 
            color='blue', label='mantle = '+str(len(data.E[data.density == 3])))
plt.scatter(data.radius[data.density == 7],data.dadt[data.density == 7], 
            color='red', label='core = '+str(len(data.E[data.density == 7])))
plt.legend()
plt.xlabel('radius [km]', fontsize=20)
plt.ylabel('da/dt [AU/Myr]', fontsize=20)
plt.ylim(min(data.dadt),max(data.dadt))
data.to_csv('synthetic_differentiated_family.csv')<jupyter_output><empty_output>
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