| [404] | 1 | def ls2sol(lstabin): |
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| 2 | |
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| 3 | # Returns solar longitude, Ls (in deg.), from day number (in sol), |
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| 4 | # where sol=0=Ls=0 at the northern hemisphere spring equinox |
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| 5 | import numpy as np |
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| 6 | import math as m |
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| 7 | |
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| 8 | year_day=668.6 |
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| 9 | peri_day=485.35 |
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| 10 | timeperi=1.90258341759902 |
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| 11 | e_elips=0.0934 |
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| 12 | pi=3.14159265358979 |
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| 13 | degrad=57.2957795130823 |
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| 14 | |
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| 15 | if type(lstabin).__name__ in ['int','float']: |
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| 16 | lstab=[lstabin] |
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| 17 | lsout=np.zeros([1]) |
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| 18 | else: |
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| 19 | lstab=lstabin |
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| 20 | lsout=np.zeros([len(lstab)]) |
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| 21 | |
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| 22 | i=0 |
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| 23 | for ls in lstab: |
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| 24 | if (np.abs(ls) < 1.0e-5): |
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| 25 | if (ls >= 0.0): |
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| 26 | ls2sol = 0.0 |
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| 27 | else: |
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| 28 | ls2sol = year_day |
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| 29 | else: |
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| 30 | |
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| 31 | zteta = ls/degrad + timeperi |
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| 32 | zx0 = 2.0*m.atan(m.tan(0.5*zteta)/m.sqrt((1.+e_elips)/(1.-e_elips))) |
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| 33 | xref = zx0-e_elips*m.sin(zx0) |
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| 34 | zz = xref/(2.*pi) |
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| 35 | ls2sol = zz*year_day + peri_day |
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| 36 | if (ls2sol < 0.0): ls2sol = ls2sol + year_day |
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| 37 | if (ls2sol >= year_day): ls2sol = ls2sol - year_day |
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| 38 | |
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| 39 | lsout[i]=ls2sol |
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| 40 | i=i+1 |
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| 41 | |
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| 42 | return lsout |
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| 43 | |
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| 44 | def sol2ls(soltabin): |
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| 45 | |
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| 46 | # convert a given martian day number (sol) |
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| 47 | # into corresponding solar longitude, Ls (in degr.), |
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| 48 | # where sol=0=Ls=0 is the |
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| 49 | # northern hemisphere spring equinox. |
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| 50 | import numpy as np |
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| 51 | import math as m |
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| 52 | |
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| 53 | year_day=668.6 |
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| 54 | peri_day=485.35 |
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| 55 | e_elips=0.09340 |
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| 56 | radtodeg=57.2957795130823 |
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| 57 | timeperi=1.90258341759902 |
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| 58 | |
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| [673] | 59 | if type(soltabin).__name__ in ['int','float','float32']: |
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| [404] | 60 | soltab=[soltabin] |
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| 61 | solout=np.zeros([1]) |
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| 62 | else: |
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| 63 | soltab=soltabin |
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| 64 | solout=np.zeros([len(soltab)]) |
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| 65 | |
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| 66 | i=0 |
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| 67 | for sol in soltab: |
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| 68 | zz=(sol-peri_day)/year_day |
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| 69 | zanom=2.*np.pi*(zz-np.floor(zz)) |
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| 70 | xref=np.abs(zanom) |
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| 71 | |
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| 72 | # The equation zx0 - e * sin (zx0) = xref, solved by Newton |
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| 73 | zx0=xref+e_elips*m.sin(xref) |
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| 74 | iter=0 |
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| 75 | while iter <= 10: |
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| 76 | iter=iter+1 |
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| 77 | zdx=-(zx0-e_elips*m.sin(zx0)-xref)/(1.-e_elips*m.cos(zx0)) |
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| 78 | if(np.abs(zdx) <= (1.e-7)): |
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| 79 | continue |
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| 80 | zx0=zx0+zdx |
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| 81 | zx0=zx0+zdx |
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| 82 | |
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| 83 | if(zanom < 0.): zx0=-zx0 |
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| 84 | # compute true anomaly zteta, now that eccentric anomaly zx0 is known |
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| 85 | zteta=2.*m.atan(m.sqrt((1.+e_elips)/(1.-e_elips))*m.tan(zx0/2.)) |
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| 86 | |
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| 87 | # compute Ls |
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| 88 | ls=zteta-timeperi |
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| 89 | if(ls < 0.): ls=ls+2.*np.pi |
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| 90 | if(ls > 2.*np.pi): ls=ls-2.*np.pi |
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| 91 | # convert Ls in deg. |
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| 92 | ls=radtodeg*ls |
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| 93 | solout[i]=ls |
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| 94 | i=i+1 |
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| 95 | |
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| 96 | return solout |
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