예제 #1
0
def profile(eos,
            energy_center,
            number=200,
            initr=0.001,
            energy_0=1e7,
            rad_0=False):
    '''Calculate the enthalpy profile of a neutron star with equation of
    state eos and central energy density energy_center in g/cm^3

    optional arguments:
        
        number: number of points

        initr: size of central seed

        energy_0: energy density at which to stop resolving crust. This doesn't
            need to be tiny (and may cause problems if it is). Integration still
            goes to surface.

        rad_0: Set true to calculate outer radius at energy_0 instead of at
        formal zero enthalpy limit of EOS
    
    '''

    # set up a core with small initial radius and mass
    initm = 4.0 / 3.0 * np.pi * (initr)**3 * energy_center * Gcc
    init_rm = np.array([initr, initm])

    # central enthalpy
    enth_c = eos.enthalpy(energy_center)

    # end the core spacing here
    enth_0 = eos.enthalpy(energy_center / 10)

    # resolve core with linear spacing in enthalpy
    linenths = np.linspace(enth_c, enth_0, number / 2)[:-1]

    # end the crust spacing here and jump to 0
    enth_0 = eos.enthalpy(energy_0)
    # resolve crust with log spacing in enthalpy
    logenths = np.logspace(np.log10(linenths[-1]), np.log10(enth_0),
                           number / 2 + 1)[1:]

    # set of enthalpies to calculate energy density, radius, and mass at
    if rad_0:
        enths = np.hstack((np.array(linenths), np.array(logenths)))
    else:
        enths = np.hstack(
            (np.array(linenths), np.array(logenths), np.array(0)))
    # enths = np.linspace(enth_c, 0, number) # boring way for debugging

    # integrate the TOV equations specified in deriv above
    rms = integrate.odeint(deriv, init_rm, enths, args=(eos, ))

    return np.vstack((enths, np.transpose(rms)))
예제 #2
0
파일: tov.py 프로젝트: jsread/nsstruc
def profile(eos, energy_center , number=200, initr=0.001, energy_0=1e7,
        rad_0=False):
    '''Calculate the enthalpy profile of a neutron star with equation of
    state eos and central energy density energy_center in g/cm^3

    optional arguments:
        
        number: number of points

        initr: size of central seed

        energy_0: energy density at which to stop resolving crust. This doesn't
            need to be tiny (and may cause problems if it is). Integration still
            goes to surface.

        rad_0: Set true to calculate outer radius at energy_0 instead of at
        formal zero enthalpy limit of EOS
    
    '''

    # set up a core with small initial radius and mass
    initm = 4.0/3.0*np.pi*(initr)**3 * energy_center * Gcc
    init_rm = np.array([initr,initm])

    # central enthalpy
    enth_c = eos.enthalpy(energy_center)

    # end the core spacing here 
    enth_0 = eos.enthalpy(energy_center/10) 

    # resolve core with linear spacing in enthalpy
    linenths = np.linspace(enth_c, enth_0, number/2)[:-1]

    # end the crust spacing here and jump to 0
    enth_0 = eos.enthalpy(energy_0) 
    # resolve crust with log spacing in enthalpy
    logenths = np.logspace(np.log10(linenths[-1]),np.log10(enth_0),
                           number/2+1)[1:]

    # set of enthalpies to calculate energy density, radius, and mass at
    if rad_0:
        enths = np.hstack((np.array(linenths),np.array(logenths)))
    else:
        enths = np.hstack((np.array(linenths),np.array(logenths),np.array(0)))
    # enths = np.linspace(enth_c, 0, number) # boring way for debugging

    # integrate the TOV equations specified in deriv above
    rms = integrate.odeint(deriv, init_rm, enths, args=(eos,))

    return np.vstack((enths,np.transpose(rms)))
예제 #3
0
def rotprofile(eos, energy_center, number=100, initr=0.001, energy_0=1e7):
    '''Calculate the enthalpy profile of a slowly rotating neutron star with
    equation of state eos and central energy density energy_center in g/cm^3.

    optional arguments:
        
        number: number of points

        initr: size of central seed

        energy_0: energy density at which to stop resolving crust. This doesn't
            need to be tiny (and may cause problems if it is). Integration still
            goes to surface.
    
    '''
    #TODO: consolodate the profile functions; this mostly just repeats
    #profile but with different initial conditions

    # central enthalpy and density
    enth_c = eos.enthalpy(energy_center)
    dens_c = eos.density(enth_c)

    # set up a core with small initial radius and mass
    initm = 4.0 / 3.0 * np.pi * (initr)**3 * energy_center * Gcc
    initma = 4.0 / 3.0 * np.pi * (initr)**3 * dens_c * Gcc

    init_rm = np.array([initr, initm, initma, 0.0, 1.0])

    # resolve core with linear spacing
    linenths = np.linspace(enth_c, enth_c / 10, number)[:-1]

    # resolve crust with log enth spacing
    enth_0 = eos.enthalpy(energy_0)  # end the crust spacing here and jump to 0
    logenths = np.logspace(np.log10(linenths[-1]), np.log10(enth_0),
                           number / 2 + 1)

    # set of enthalpies to calculate energy density, radius, and mass at
    enths = np.hstack(
        (np.array(linenths), np.array(logenths[1:]), np.array(0)))
    # enths = np.linspace(enth_c, 0, number) # boring way for debugging

    # integrate the TOV equations specified in deriv above
    rms = integrate.odeint(rotderiv, init_rm, enths, args=(eos, ))

    return np.vstack((enths, np.transpose(rms)))
예제 #4
0
파일: tov.py 프로젝트: jsread/nsstruc
def rotprofile(eos, energy_center , number=100, initr=0.001, energy_0=1e7):
    '''Calculate the enthalpy profile of a slowly rotating neutron star with
    equation of state eos and central energy density energy_center in g/cm^3.

    optional arguments:
        
        number: number of points

        initr: size of central seed

        energy_0: energy density at which to stop resolving crust. This doesn't
            need to be tiny (and may cause problems if it is). Integration still
            goes to surface.
    
    '''
    #TODO: consolodate the profile functions; this mostly just repeats
    #profile but with different initial conditions

    # central enthalpy and density
    enth_c = eos.enthalpy(energy_center)
    dens_c = eos.density(enth_c)

 
    # set up a core with small initial radius and mass
    initm = 4.0/3.0*np.pi*(initr)**3 * energy_center * Gcc
    initma = 4.0/3.0*np.pi*(initr)**3 * dens_c * Gcc

    init_rm = np.array([initr,initm, initma, 0.0, 1.0])

    # resolve core with linear spacing
    linenths = np.linspace(enth_c, enth_c/10, number)[:-1]

    # resolve crust with log enth spacing
    enth_0 = eos.enthalpy(energy_0) # end the crust spacing here and jump to 0
    logenths = np.logspace(np.log10(linenths[-1]),np.log10(enth_0),
                           number/2+1)

    # set of enthalpies to calculate energy density, radius, and mass at
    enths = np.hstack((np.array(linenths),np.array(logenths[1:]),np.array(0)))
    # enths = np.linspace(enth_c, 0, number) # boring way for debugging

    # integrate the TOV equations specified in deriv above
    rms = integrate.odeint(rotderiv, init_rm, enths, args=(eos,))

    return np.vstack((enths,np.transpose(rms)))