Going to Jupiter with Python using Jupyter and poliastro

In [1]:

    

import numpy as np
import matplotlib.pyplot as plt
plt.ion()

import astropy.units as u
from astropy.time import Time
from astropy.coordinates import solar_system_ephemeris

from poliastro.bodies import Sun, Earth, Jupiter
from poliastro.twobody import Orbit
from poliastro.maneuver import Maneuver
from poliastro.iod import izzo
from poliastro.plotting import plot, OrbitPlotter
from poliastro.util import norm

solar_system_ephemeris.set("jpl")


    

    
Out[1]:





<ScienceState solar_system_ephemeris: 'jpl'>

In [2]:

    

## Initial data
# Links and sources: https://github.com/poliastro/poliastro/wiki/EuroPython:-Per-Python-ad-Astra
date_launch = Time("2011-08-05 16:25", scale='utc')
C_3 = 31.1 * u.km**2 / u.s**2
date_flyby = Time("2013-10-09 19:21", scale='utc')
date_arrival = Time("2016-07-05 03:18", scale='utc')


    

In [3]:

    

# Initial state of the Earth
ss_e0 = Orbit.from_body_ephem(Earth, date_launch)
r_e0, v_e0 = ss_e0.rv()


    

In [4]:

    

r_e0


    

    
Out[4]:





$[1.0246553 \times 10^{8},~-1.023135 \times 10^{8},~-44353346] \; \mathrm{km}$

In [5]:

    

v_e0


    

    
Out[5]:





$[1847708.5,~1594323.4,~691089.12] \; \mathrm{\frac{km}{d}}$

In [6]:

    

# State of the Earth the day of the flyby
ss_efly = Orbit.from_body_ephem(Earth, date_flyby)
r_efly, v_efly = ss_efly.rv()


    

In [7]:

    

# Assume that the insertion velocity is tangential to that of the Earth
dv = C_3**.5 * v_e0 / norm(v_e0)
man = Maneuver.impulse(dv)


    

In [8]:

    

# Inner Cruise 1
ic1 = ss_e0.apply_maneuver(man)
ic1.rv()


    

    
Out[8]:





(<Quantity [  1.02465527e+08, -1.02313505e+08, -4.43533465e+07] km>,
 <Quantity [ 2198705.82621214, 1897186.74383867,  822370.88977492] km / d>)

In [9]:

    

ic1.period.to(u.year)


    

    
Out[9]:





$2.1515474 \; \mathrm{yr}$

In [10]:

    

op = OrbitPlotter()

op.plot(ss_e0)
op.plot(ic1)


    

    
Out[10]:





[<matplotlib.lines.Line2D at 0x22d5f6f7390>,
 <matplotlib.lines.Line2D at 0x22d5f6f7fd0>]






    

In [11]:

    

# We propagate until the aphelion
ss_aph = ic1.propagate(ic1.period / 2)
ss_aph.epoch


    

    
Out[11]:





<Time object: scale='utc' format='iso' value=2012-09-01 14:38:54.507>

In [12]:

    

# Let's compute the Lambert solution to do the flyby of the Earth
time_of_flight = date_flyby - ss_aph.epoch
time_of_flight


    

    
Out[12]:





<TimeDelta object: scale='tai' format='jd' value=403.19589691198047>

In [13]:

    

(v_aph, v_fly), = izzo.lambert(Sun.k, ss_aph.r, ss_efly.r, time_of_flight)


    

In [14]:

    

# Check the delta-V
norm(v_aph - ss_aph.v)  # Too high!


    

    
Out[14]:





$1.079866 \; \mathrm{\frac{km}{s}}$

In [15]:

    

ss_aph_post = Orbit.from_vectors(Sun, ss_aph.r, v_aph, epoch=ss_aph.epoch)
ss_junofly = Orbit.from_vectors(Sun, r_efly, v_fly, epoch=date_flyby)


    

In [16]:

    

op = OrbitPlotter()

op.plot(ss_e0, label="Earth")
op.plot(ic1, label="Inner Cruise 1")
#op.plot(ss_efly)
op.plot(ss_aph_post, label="Back to Earth")


    

    
Out[16]:





[<matplotlib.lines.Line2D at 0x22d612d8630>,
 <matplotlib.lines.Line2D at 0x22d612d8c18>]






    

In [17]:

    

# And now, go to Jupiter!
ss_j = Orbit.from_body_ephem(Jupiter, date_arrival)
r_j, v_j = ss_j.rv()


    

In [18]:

    

(v_flypre, v_oip), = izzo.lambert(Sun.k, r_efly, r_j, date_arrival - date_flyby)


    

In [19]:

    

ss_oip = Orbit.from_vectors(Sun, r_j, v_oip, epoch=date_flyby)


    

In [20]:

    

fig, ax = plt.subplots(figsize=(9, 12))

op = OrbitPlotter(ax)

op.plot(ss_e0, label="Earth")
op.plot(ic1, label="Inner Cruise 1")
#op.plot(ss_efly)
op.plot(ss_aph_post, label="Back to Earth")
op.plot(ss_oip, label="Jupiter Orbit Insertion Phase")
op.plot(ss_j, label="Jupiter")

fig.savefig("jupiter.png")