Phase_curve_TTV module

Phase_curve_TTV.phase_TTV(P_TTV, t0, t_end, transit_peaks, nb_points)

Computes the phase of the planet taking into account the modification of the period due to TTVs starting from the nearest transit peak from t0

Parameters:

  • P_TTV (numpy.ndarray) – the modified orbital periods of the planet due to the TTVs (in days)

  • t0 (float) – the initial time (in BJD_TBD - 2450000)

  • t_end (float) – the final time (in BJD_TBD - 2450000)

  • transit_peaks (numpy.ndarray) – the peaks of the transits (in BJD_TBD - 2450000)

  • nb_points (int) – the number of points for the phase curve

Returns:

phases_TTV, t

Return type:

numpy.ndarray, numpy.ndarray

Phase_curve_TTV.phase_curve_simulation(t0, nb_days, nb_points=10000, planets='bcdefgh', redistribution=0, filter=None, model='sphinx', unit='ppm', Keplerian=False, total=True, plot=True, save_plot=False, save_txt=False)

Simulates the phase curves of the planets of TRAPPIST-1 for a given number of days starting from t0 taking into account the modified periods due to TTVs. We assume circular orbits as otherwise the code does not manage to solve the Kepler equation to compute the true anomaly due to the modified periods.

Parameters:

  • t0 (float) – the initial time (in BJD_TBD - 2450000)

  • nb_days (int) – the number of days to simulate

  • nb_points (int) – the number of points for the phase curves (default: 10000)

  • planets (str) – the planets to simulate (default: ‘bcdefgh’)

  • redistribution (float) – the redistribution efficiency between the day side and night side (default: 0)

  • filter (str or None) – the filter to use (default: None). If None, the bolometric fluxes, expressed in ppm, are used relatively to the stellar flux with the planets considered as bare rocks.

  • model (str) – the model to use for the stellar flux (default: ‘sphinx’). If ‘sphinx’, the flux is computed using the SPHINX model. If ‘phoenix’, the flux is computed using the PHOENIX model.

  • unit (str) – the unit of the phase curve (default: ‘ppm’). If ‘ppm’, the fluxes of the planets will be computed relatively to the stellar flux in ppm. If ‘mJy’, the planetary fluxes will be computed in absolute value in “mJy”. Will be set automatically to ‘mJy’ if the model is ‘phoenix’.

  • Keplerian (bool) – whether to use the Keplerian periods or not (default: False)

  • total (bool) – whether to plot the total phase curve or not (default: True)

  • plot (bool) – whether to plot the phase curves or not (default: True)

  • save_plot (bool) – whether to save the plot or not (default: False)

  • save_txt (bool) – whether to save the phase curves as txt files or not (default: False)

Returns:

None

Phase_curve_TTV.main()