# Source code for spacepy.empiricals

    #!/usr/bin/env python
    # -*- coding: utf-8 -*-
    """
    Module with some useful empirical models (plasmapause, magnetopause, Lmax)

    Authors: Steve Morley, Josef Koller
    Institution: Los Alamos National Laboratory
    Contact: smorley@lanl.gov

    Copyright 2010 Los Alamos National Security, LLC.
    """
    from __future__ import division
    import datetime
    from functools import partial
    import numpy as np

    import scipy.integrate as integ
    from spacepy import help
    import spacepy.datamodel as dm
    import spacepy.toolbox as tb
    import spacepy.omni as om
    import spacepy.time as spt

    __contact__ = 'Steve Morley, smorley@lanl.gov'

    def getLmax(ticks, model='JKemp', dbase='QDhourly'):
        """
        calculate a simple empirical model for Lmax - last closed drift-shell

        Uses the parametrized Lmax from:
        Koller and Morley (2010)
        'Magnetopause shadowing effects for radiation belt models during high-speed solar wind streams'
        American Geophysical Union, Fall Meeting 2010, abstract #SM13A-1787

        Parameters
        ==========
        ticks : spacepy.time.Ticktock
            Ticktock object of desired times
        model : string, optional
            'JKemp' (default - empirical model of J. Koller)

        Returns
        =======
        out : np.ndarray
            Lmax - L* of last closed drift shell

        Examples
        ========
        >>> from spacepy.empiricals import getLmax
        >>> import spacepy.time as st
        >>> import datetime
        >>> ticks = st.tickrange(datetime.datetime(2000, 1, 1), datetime.datetime(2000, 1, 3), deltadays=1)
        array([ 7.4928412,  8.3585632,  8.6463423])

        See Also
        ========
        spacepy.LANLstar.LANLmax

        """
        omni = om.get_omni(ticks, dbase=dbase)
        Dst = omni['Dst']
        Lmax = np.zeros(len(Dst))
        if model == 'JKemp':
            for i, iDst in enumerate(Dst):
                Lmax[i] = 6.07e-5*iDst*iDst + 0.0436*iDst + 9.37
        else:
            raise ValueError('Invalid model selection')
        return Lmax

    def getPlasmaPause(ticks, model='M2002', LT='all', omnivals=None):
        """
        Plasmapause location model(s)

        CA1992 -- Carpenter, D. L., and R. R. Anderson, An ISEE/whistler
        model of equatorial electron density in the magnetosphere,
        J. Geophys. Res., 97, 1097, 1992.
        M2002 -- Moldwin, M. B., L. Downward, H. K. Rassoul, R. Amin,
        and R. R. Anderson, A new model of the location of the plasmapause:
        CRRES results, J. Geophys. Res., 107(A11), 1339,
        doi:10.1029/2001JA009211, 2002.
        RT1970 -- Rycroft, M. J., and J. O. Thomas, The magnetospheric
        plasmapause and the electron density trough at the alouette i
        orbit, Planetary and Space Science, 18(1), 65-80, 1970

        Parameters
        ==========
        ticks : spacepy.time.Ticktock
            TickTock object of desired times
        Lpp_model : string, optional
            'CA1992' or 'M2002' (default)
            CA1992 returns the Carpenter and Anderson model,
            M2002 returns the Moldwin et al. model
        LT : int, float
            requested local time sector, 'all' is valid option
        omnivals : spacepy.datamodel.SpaceData, dict
            dict-like containing UTC (datetimes) and Kp keys

        Returns
        =======
        out : float
            Plasmapause radius in Earth radii

        Examples
        ========
        >>> import spacepy.time as spt
        >>> import spacepy.empiricals as emp
        >>> ticks = spt.tickrange('2002-01-01T12:00:00','2002-01-04T00:00:00',.25)
        >>> emp.getPlasmaPause(ticks)
        array([ 6.42140002,  6.42140002,  6.42140002,  6.42140002,  6.42140002,
            6.42140002,  6.42140002,  6.26859998,  5.772     ,  5.6574    ,
            5.6574    ])
        """
        def calcLpp(Kpmax, A, B, power=1):
            currLpp = A - B*Kpmax**power
            return currLpp

        model_list = ['CA1992', 'M2002', 'RT1970']

        if model == 'CA1992':
            if LT!='all':
                print('No LT dependence currently supported for this model')
        if model not in model_list:
            raise ValueError("Please specify a valid model:\n{0}".format(' or '.join(model_list)))

        if LT=='all':
            parA = {'CA1992': 5.6,  'M2002': 5.39,  'RT1970': 5.64}
            parB = {'CA1992': 0.46, 'M2002': 0.382, 'RT1970': 0.78}
            priorvals = {'CA1992': datetime.timedelta(hours=24),
                         'M2002': datetime.timedelta(hours=12),
                         'RT1970': datetime.timedelta(0)}
            A, B = parA[model], parB[model]
            prior = priorvals[model]
        else:
            try:
                float(LT)
            except (ValueError, TypeError):
                raise ValueError("Please specify a valid LT:\n'all' or a numeric type")
            parA = {'CA1992': [5.6]*24,
                    'M2002': [5.7]*3+[6.05]*6+[5.2]*6+[4.45]*6+[5.7]*3,
                    'RT1970': [5.64]*24}
            parB = {'CA1992': [0.46]*24,
                    'M2002': [0.42]*3+[0.573]*6+[0.425]*6+[0.167]*6+[0.42]*3,
                    'RT1970': [0.78]*24}
            priorvals = {'CA1992': [datetime.timedelta(hours=24)]*24,
                         'M2002': [datetime.timedelta(hours=12)]*24,
                         'RT1970': [datetime.timedelta(0)]*24}
            try:
                LThr = long(LT)
            except NameError:
                LThr = int(LT)
            prior = priorvals[model][LThr]
            A, B = parA[model][LThr], parB[model][LThr]

        st, en = ticks.UTC[0]-prior, ticks.UTC[-1]
        if omnivals is None:
            omdat = om.get_omni(spt.tickrange(st, en, 1.0/24.0), dbase='QDhourly')
        else:
            #now test for sanity of input
            try:
                assert isinstance(omnivals, dict)
            except:
                raise TypeError('Not a valid input type for omnivals, expected spacepy.datamodel.SpaceData')
            try:
                assert 'UTC' in omnivals
                assert 'Kp' in omnivals
            except:
                raise KeyError('Required data not found in input dict-like (omnivals)')
            omdat = omnivals

        einds, oinds = tb.tOverlap([st, en], omdat['UTC'])
        utc = np.array(omdat['UTC'])[oinds]
        Kp = np.array(omdat['Kp'])[oinds]
        Lpp = np.zeros(len(ticks))

        if model == 'RT1970':
            power = 0.5
        else:
            power = 1
        for i, t1 in enumerate(ticks.UTC):
            t0 = t1-prior
            iprevday, dum = tb.tOverlap(utc, [t0, t1])
            if iprevday:
                Kpmax = max(Kp[iprevday])
                Lpp[i] = calcLpp(Kpmax, A, B, power=power)
            else:
                Lpp[i] = np.nan

        return Lpp

    def getMagnetopause(ticks, LTs=None, dbase='QDhourly'):
        '''Calculates the Shue et al. (1997) position in equatorial plane

        Shue et al. (1997), A new functional form to study the solar wind
        control of the magnetopause size and shape, J. Geophys. Res., 102(A5),
        9497–9511, doi:10.1029/97JA00196.

        Parameters
        ==========
        ticks : spacepy.time.Ticktock
            TickTock object of desired times (will be interpolated from hourly OMNI data)
            OR dictionary of form {'P': [], 'Bz': []}
            Where P is SW ram pressure [nPa] and Bz is IMF Bz (GSM) [nT]
        LTs : array-like
            Array-like of local times for evaluating the magnetopause model. Default is
            6 LT to 18 LT in steps of 20 minutes.

        Returns
        =======
        out : array
            NxMx2 array of magnetopause positions [Re]
            N is number of timesteps, M is number of local times. The 2 positions
            are the X_GSE and Y_GSE positions of the magnetopause

        Examples
        ========
        >>> import spacepy.time as spt
        >>> import spacepy.empiricals as emp
        >>> ticks = spt.Ticktock(['2002-01-01T12:00:00','2002-01-04T00:00:00'])
        >>> localtimes = [13,12,11]
        >>> emp.getMagnetopause(ticks, LTs=localtimes)
        array([[[ 10.27674331,  -2.75364507],
            [ 10.52909163,   0.        ],
            [ 10.27674331,   2.75364507]],
           [[ 10.91791834,  -2.9254474 ],
            [ 11.18712131,   0.        ],
            [ 10.91791834,   2.9254474 ]]])
        >>> emp.getMPstandoff(ticks) #should give same result as getMagnetopause for 12LT
        array([ 10.52909163,  11.18712131])

        To plot the magnetopause:
        >>> import numpy as np
        >>> import spacepy.plot as splot
        >>> import matplotlib.pyplot as plt
        >>> localtimes = np.arange(5, 19.1, 0.5)
        >>> mp_pos = emp.getMagnetopause(ticks, localtimes)
        >>> plt.plot(mp_pos[0,:,0], mp_pos[0,:,1])
        >>> ax1 = plt.gca()
        >>> ax1.set_xlim([-5,20])
        >>> ax1.set_xlabel('X$_{GSE}$ [R$_E$]')
        >>> ax1.set_ylabel('Y$_{GSE}$ [R$_E$]')
        >>> splot.dual_half_circle(ax=ax1)
        >>> ax1.axes.set_aspect('equal')

        '''

        alpha = []
        r0 = getMPstandoff(ticks, dbase=dbase, alpha=alpha)
        alpha = np.asarray(alpha)

        if LTs is None:
            LTs = np.arange(6, 18.1, 1/3.0)

        r = np.zeros([len(ticks),len(LTs)])
        out = np.zeros([len(ticks),len(LTs), 2])

        angs = (12.0-np.asanyarray(LTs))*15.0

        costheta = np.cos(np.deg2rad(angs))
        sintheta = np.sin(np.deg2rad(angs))
        for idx, ct in enumerate(costheta):
            r[:,idx] = r0 * (2.0/(1+ct))**alpha
        out[:,:,0] = r*costheta #Xgse
        out[:,:,1] = r*sintheta #Ygse

        return out

    def getMPstandoff(ticks, dbase='QDhourly', alpha=[]):
        """Calculates the Shue et al. (1997) subsolar magnetopause radius

        Shue et al. (1997), A new functional form to study the solar wind
        control of the magnetopause size and shape, J. Geophys. Res., 102(A5),
        9497–9511, doi:10.1029/97JA00196.

        Parameters
        ==========
        ticks : spacepy.time.Ticktock
            TickTock object of desired times (will be interpolated from hourly OMNI data)
            OR dictionary of form {'P': [], 'Bz': []}
            Where P is SW ram pressure [nPa] and Bz is IMF Bz (GSM) [nT]
        alpha : list
            Used as an optional return value to obtain the flaring angles. To use, assign
            an empty list and pass to this function through the keyword argument. The list
            will be modified in place, adding the flaring angles for each time step.

        Returns
        =======
        out : float
            Magnetopause (sub-solar point) standoff distance [Re]

        Examples
        ========
        >>> import spacepy.time as spt
        >>> import spacepy.empiricals as emp
        >>> ticks = spt.tickrange('2002-01-01T12:00:00','2002-01-04T00:00:00',.25)
        >>> emp.getMPstandoff(ticks)
        array([ 10.57319537,  10.91327764,  10.75086873,  10.77577207,
             9.78180261,  11.0374474 ,  11.4065    ,  11.27555451,
            11.47988573,  11.8202582 ,  11.23834814])
        >>> data = {'P': [2,4], 'Bz': [-2.4, -2.4]}
        >>> emp.getMPstandoff(data)
        array([ 9.96096838,  8.96790412])
        """
        if type(ticks) == spt.Ticktock:
            omni = om.get_omni(ticks, dbase=dbase)
            P, Bz = omni['Pdyn'], omni['BzIMF']
        elif isinstance(ticks, dict):
            P, Bz = ticks['P'], ticks['Bz']
            try:
                len(P)
            except TypeError:
                P = [P]
            try:
                len(Bz)
            except TypeError:
                Bz = [Bz]
        else:
            raise(TypeError('Invalid Input type'))

        try:
            # Initialize r0 and make P and Bz numpy arrays
            r0 = np.zeros((len(P)), dtype=float)
            Bz = np.array(Bz)
            P = np.array(P)

            # Find where Bz >= 0 and where it is < 0
            iBzPos = np.where(Bz >= 0)
            iBzNeg = np.where(Bz < 0)

            # Calculate r0
            r0[iBzPos] = (11.4 + 0.013*Bz[iBzPos])*P[iBzPos]**(-1/6.6)
            r0[iBzNeg] = (11.4 + 0.140*Bz[iBzNeg])*P[iBzNeg]**(-1/6.6)
            flarang = (0.58 - 0.01*Bz)*(1.0 + 0.01*P)
            alpha.extend(flarang)

            return r0
        except TypeError:
            raise TypeError("Please check for valid input types")

    def getDststar(ticks, model='OBrien', dbase='QDhourly'):
        """Calculate the pressure-corrected Dst index, Dst*

        We need to add in the references to the models here!

        Parameters
        ==========
        ticks : spacepy.time.Ticktock
            TickTock object of desired times (will be interpolated from hourly OMNI data)
            OR dictionary including 'Pdyn' and 'Dst' keys where data are lists or arrays
            and Dst is in [nT], and Pdyn is in [nPa]

        Returns
        =======
        out : float
            Dst* - the pressure corrected Dst index from OMNI [nT]

        Examples
        ========
        Coefficients are applied to the standard formulation e.g. Burton et al., 1975
        of Dst* = Dst - b*sqrt(Pdyn) + c
        The default is the O'Brien and McPherron model (2002).
        Other options are Burton et al. (1975) and Borovsky and Denton (2010)

        >>> import spacepy.time as spt
        >>> import spacepy.omni as om
        >>> import spacepy.empiricals as emp
        >>> ticks = spt.tickrange('2000-10-16T00:00:00', '2000-10-31T12:00:00', 1/24.)
        >>> dststar = emp.getDststar(ticks)
        >>> dststar[0]
        -21.317220132108943

        User-determined coefficients can also be supplied as a two-element list
        or tuple of the form (b,c), e.g.

        >>> dststar = emp.getDststar(ticks, model=(2,11)) #b is extreme driving from O'Brien

        We have chosen the OBrien model as the default here as this was rigorously
        determined from a very long data set and is pertinent to most conditions.
        It is, however, the most conservative correction. Additionally, Siscoe,
        McPherron and Jordanova (2005) argue that the pressure contribution to Dst diminishes
        during magnetic storms.

        To show the relative differences, run the following example:

        >>> import matplotlib.pyplot as plt
        >>> params = [('Burton','k-'), ('OBrien','r-'), ('Borovsky','b-')]
        >>> for model, col in params:
                dststar = getDststar(ticks, model=model)
                plt.plot(ticks.UTC, dststar, col)

        """
        model_params = {'Burton': (15.8, 20),
                        'OBrien': (7.26, 11),
                        'Borovsky': (20.7,27.7)}

        if isinstance(model, str):
            try:
                b, c = model_params[model]
            except KeyError:
                raise ValueError('Invalid pressure correction model selected')
        else:
            try:
                b, c = model[0], model[1]
            except (KeyError, IndexError):
                raise ValueError('Invalid coefficients set: must be of form (b,c)')

        if isinstance(ticks, spt.Ticktock):
            omni = om.get_omni(ticks, dbase=dbase)
            P, Dst = omni['Pdyn'], omni['Dst']
        elif isinstance(ticks, dict):
            P, Dst = ticks['Pdyn'], ticks['Dst']
            if isinstance(P, list):
                P, Dst = np.array(P), np.array(Dst)

        #get Dst*
        Dststar = Dst - b*P**0.5 + c

        return Dststar

    def getExpectedSWTemp(velo, model='XB15', units='K'):
        '''Return the expected solar wind temperature based on the bulk velocity

        The formulations used by this function are those given by,
        L87  -- Lopez, R.E., J. Geophys. Res., 92, 11189-11194, 1987
        BS06 -- Borovsky, J.E. and J.T. Steinberg, Geophysical Monograph Series 167, 59-76, 2006
        XB15 -- Xu, F. and J.E. Borovsky, J. Geophys. Res., 120, 70-100, 2015

        Parameters
        ==========
        velo : array-like
            Array like of solar wind bulk velocity values [km/s]

        model : str [optional]
            Name of model to use. Valid choices are L87, BS06 and XB15. Default is XB15

        units : str [optional]
            Units for output temperature, options are eV or K. Default is Kelvin [K]

        Returns
        =======
        Texp : array-like
            The expected solar wind temperature given the bulk velocity [K] or [eV]

        '''
        v = np.asanyarray(velo)
        def bs06(v):
            '''Borovsky and Steinberg 2006, Geophysical Monograph - median values'''
            Texp = np.empty(len(v))
            Texp.fill(np.nan)
            Texp[v<372]  = 1.28e-8*v[v<372]**3.324
            Texp[v>=372] = 0.0572*v[v>=372] - 16.79
            return Texp

        def xb15(v):
            '''Xu and Borovsky 2015, JGR'''
            Texp = (v/258.0)**3.113
            return Texp

        def l87(v):
            '''Lopez 1987, JGR - Tables 1&2 [T(V)] from IMP-8'''
            Texp = np.empty(len(v))
            Texp.fill(np.nan)
            Texp[v<500]  = (0.031*v[v<500] - 5.1)**2
            Texp[v>=500] = (0.02*v[v>=500] + 0.5)**2
            return Texp*1e3/1.16045221e4 #return in eV

        formulae = {'BS06': bs06, 'XB15': xb15, 'L87': l87}

        try:
            mod = model.upper()
            Texp = formulae[mod](v)
        except KeyError:
            raise KeyError('Invalid model specified for SW temperature')

        if units.lower()=='k':
            return Texp*1.16045221e4
        elif units.lower()=='ev':
            return Texp
        else:
            raise ValueError('Invalid units specified for SW temperature, must be "K" or "eV"')

    def vampolaPA(omniflux, **kwargs):
        '''Pitch angle model of sin^n form

        Parameters
        ==========
        omniflux : arraylike or float
            omnidirectional number flux data

        order : integer or float (optional)
            order of sin^n functional form for distribution (default=2)

        alphas : arraylike (optional)
            pitch angles at which to evaluate the differential number flux
            (default is 5 to 90 degrees in 36 steps)

        Returns
        =======
        dnflux : array
            differential number flux corresponding to pitch angles alphas
        alphas : array
            pitch angles at which the differential number flux was evaluated

        Examples
        ========
        Omnidirectional number flux of [3000, 6000]

        >>> from spacepy.empiricals import vampolaPA
        >>> vampolaPA(3000, alpha=[45, 90])
        (array([ 179.04931098,  358.09862196]), [45, 90])
        >>> data, pas = vampolaPA([3000, 6000], alpha=[45, 90])
        >>> pas
        [45, 90]
        >>> data
        array([[ 179.04931098,  358.09862196],
           [ 358.09862196,  716.19724391]])

        Notes
        =====
        Directional number flux integrated over pitch angle from 0 to 90 degrees
        is a factor of 4*pi lower than omnidirectional number flux.

        '''
        defaults = {'order': 2,
                    'alpha': tb.linspace(5,90,18)}

        if hasattr(omniflux, '__iter__'):
            omniflux = np.asanyarray(omniflux)
        else:
            omniflux = np.asanyarray([omniflux])

        #substitute defaults
        for key in defaults:
            if key not in kwargs:
                kwargs[key] = defaults[key]

        if hasattr(kwargs['order'], '__iter__'):
            try:
                assert len(kwargs['order'])==len(omniflux)
            except AssertionError:
                raise ValueError('order must be either single-valued or the same length as omniflux')
        else:
            kwargs['order'] = np.asanyarray([kwargs['order']]*len(omniflux))
        normfac = np.empty(len(kwargs['order']), dtype=float)

        def sinfunc(x, order=kwargs['order']): #define distribution function
            dum = np.sin(x)
            return dum**order

        for idx, tmporder in enumerate(kwargs['order']):
            sinfunc_o = partial(sinfunc, order=tmporder+1)
            normfac[idx] = omniflux[idx]/(2*np.pi*integ.quad(sinfunc_o, 0, np.pi)[0])
        #now make the differential number flux
        dnflux = np.zeros((len(kwargs['alpha']), len(omniflux))).squeeze()
        for i, a_val in enumerate(np.deg2rad(kwargs['alpha'])):
            dnflux[i] = normfac * sinfunc(a_val)

        return dnflux, kwargs['alpha']

    def getVampolaOrder(L):
        '''Empirical lookup of power for sin^n pitch angle model from Vampola (1996)

        Vampola, A.L. Outer zone energetic electron environment update,
        Final Report of ESA/ESTEC/WMA/P.O. 151351, ESA-ESTEC, Noordwijk,
        The Netherlands, 1996.

        Parameters
        ==========
        L : arraylike or float

        Returns
        =======
        order : array
            coefficient for sin^n model corresponding to McIlwain L (computed for OP77?)

        Examples
        ========
        Apply Vampola pitch angle model at L=[4, 6.6]

        >>> from spacepy.empiricals import vampolaPA, getVampolaOrder
        >>> order = getVampolaOrder([4,6.6])
        >>> order
        array([ 3.095 ,  1.6402])
        >>> vampolaPA([3000, 3000], alpha=[45, 90], order=order)
        (array([[ 140.08798878,  192.33572182],
            [ 409.49143136,  339.57417256]]), [45, 90])
        '''
        lmc = np.arange(3,8.00001,0.25)
        vamp_n = [5.38, 5.078, 4.669, 3.916, 3.095, 2.494, 2.151, 1.998, 1.899,
                  1.942, 1.974, 1.939, 1.970, 2.136, 1.775, 1.438, 1.254, 1.194,
                  1.046, 0.989, 0.852]

        if not hasattr(L, '__iter__'): L = [L]
        L = np.asanyarray(L)
        #if outside valid range, use end value
        L[L<=3] = 3
        L[L>=8] = 8
        #interpolate to get order for the given L
        order = np.interp(L, lmc, vamp_n)

        return order

    def omniFromDirectionalFlux(fluxarr, alphas, norm=True):
        '''
        Calculate omnidirectional flux [(s cm^2 kev)^-1] from directional flux [(s sr cm^2 keV)^-1] array

        J = 2.pi integ(j sin(a) da)
        If kwarg 'norm' is True (default), the omni flux is normalized by 4.pi to make it per steradian,
        in line with the PRBEM guidelines

        Parameters
        ==========
        fluxarr : arraylike
            Array of directional flux values
        alphas : arraylike
            Array of pitch angles corresponding to fluxarr

        Returns
        =======
        omniflux : float
            Omnidirectional flux value

        Examples
        ========
        Roundtrip from omni flux, to directional flux (Vampola model),
        integrate to get back to omni flux.

        >>> from spacepy.empiricals import vampolaPA, omniFromDirectionalFlux
        >>> dir_flux, pa  = vampolaPA(3000, alpha=range(0,181,2), order=4)
        >>> dir_flux[:10], pa[:10]
        (array([  0.00000000e+00,   6.64032473e-04,   1.05986545e-02,
              5.34380898e-02,   1.67932162e-01,   4.06999226e-01,
              8.36427502e-01,   1.53325140e+00,   2.58383611e+00,
              4.08170975e+00]), [0, 2, 4, 6, 8, 10, 12, 14, 16, 18])
        >>> omniFromDirectionalFlux(dir_flux, pa, norm=False)
        3000.0000008112293

        Calculate "spin-averaged" flux, giving answer per steradian

        >>> omniFromDirectionalFlux(dir_flux, pa, norm=True)
        238.73241470239859
        '''
        try:
            flen = len(fluxarr)
        except TypeError:
            fluxarr = np.array([fluxarr])
            flen = 1
        finally:
            if flen==1:
                #assume isotropy
                return fluxarr
        if norm:
           fac = 1
           denomina = integ.quad(np.sin, 0, np.pi)[0]
        else:
           fac = 2*np.pi
           denomina = 1
        alphrad = np.deg2rad(alphas)
        numera = integ.simps(fluxarr*np.sin(alphrad), alphrad)
        omniflux = fac*numera/denomina
        return omniflux

    def getSolarRotation(ticks, rtype='carrington', fp=False, reverse=False):
        '''Calculates solar rotation number (Carrington or Bartels) for a given date/time

        Parameters
        ==========
        ticks : spacepy.time.Ticktock or datetime.datetime

        Returns
        =======
        rnumber : integer or array
            Carrington (or Bartels) rotation number

        '''
        def total_seconds(dobj):
            return dobj.days*24*3600 + dobj.seconds + dobj.microseconds/1e6
        if rtype.lower() == 'carrington':
            start_date = datetime.datetime(1853,11,9,21,38,44,160000)
            #length = datetime.timedelta(days=27, minutes=396, seconds=25, microseconds=919999)
            length = datetime.timedelta(days=27.2753)
        elif rtype.lower() == 'bartels':
            start_date = datetime.datetime(1832,2,8)
            start_JD = spt.Ticktock(start_date).JD
            length = datetime.timedelta(days=27)
        else:
            raise ValueError('Solar rotation type {0} not recognized: Must be either "carrington" or "Bartels"'.format(rtype))
        if not reverse:
            try:
                nels = len(ticks)
            except TypeError:
                try:
                    rotation = total_seconds(ticks-start_date)/total_seconds(length)
                    rotation += 1
                    if not fp:
                        rotation = int(rotation)
                    return rotation
                except:
                    raise RuntimeError('Unidentified problem with input time {0} in getSolarRotation'.format(ticks))
            if isinstance(ticks, spt.Ticktock):
                rotation = [total_seconds(tt-start_date)/total_seconds(length) for tt in ticks.UTC]
                rotation = np.array(rotation) + 1
            else:
                try:
                    rotation = [total_seconds(tt-start_date)/total_seconds(length) for tt in ticks]
                    rotation = np.array(rotation) + 1
                except:
                    raise RuntimeError('Unidentified problem with input time {0} in getSolarRotation'.format(ticks))
            if not fp:
                rotation = rotation.astype(int)
            return rotation
        else:
            #for now just assume single input, non-iterable
            elapsed = length*(ticks-1)
            date = elapsed + start_date
            return date

    def getSolarProtonSpectra(norm=3.20e7, gamma=-0.96, E0=15.0, Emin=.1, Emax=600, nsteps=100):
        '''Returns a SpaceData with energy and fluence spectra of solar particle events

        The formulation follows that of:
        Ellison and Ramaty ApJ 298: 400-408, 1985
        dJ/dE = K^{-\gamma}exp(-E/E0)

        and the defualt values are the 10/16/2003 SEP event of:
        Mewaldt, R. A., et al. (2005), J. Geophys. Res., 110, A09S18, doi:10.1029/2005JA011038.

        Other Parameters
        ================
        norm : float
            Normilization factor for the intensity of the SEP event
        gamma : float
            Power law index
        E0 : float
            Expoential scaling factor
        Emin : float
            Minimum energy for fit
        Emax : float
            Maximum energy for fit
        nsteps : int
            The number of log spaced energy steps to return

        Returns
        =======
        data : dm.SpaceData
            SpaceData with the energy and fluence values
        '''
        E = tb.logspace(Emin, Emax, nsteps)
        fluence = norm*E**(gamma)*np.exp(-E/E0)
        ans = dm.SpaceData()
        ans['Energy'] = dm.dmarray(E)
        ans['Energy'].attrs = {'UNITS':'MeV',
                               'DESCRIPTION':'Particle energy per nucleon'}
        ans['Fluence'] = dm.dmarray(fluence)
        ans['Fluence'].attrs = {'UNITS' : 'cm^{-2} sr^{-1} (MeV/nuc)^{-1}',
                                'DESCRIPTION':'Fluence spectra fir to the model'}
        return ans

    ShueMP = getMPstandoff
    get_plasma_pause = getPlasmaPause
    get_Lmax = getLmax