研究目的
Determining epochs of maximum angular separation for the star and planet to aid in direct imaging of exoplanets.
研究成果
The study provides a methodology for determining the epochs of maximum angular separation for the star and planet, which is crucial for direct imaging of exoplanets. The work emphasizes the need for further radial velocity observations to reacquire the planetary location and improve orbital ephemerides for direct imaging observations.
研究不足
The challenges include coronagraph development and achieving the necessary contrast ratio for direct imaging of exoplanets. The uncertainty in the orbital location becomes comparable to the orbital period for particularly long periods, making it impossible to provide useful ephemeris information for follow-up observations.
1：Experimental Design and Method Selection:
The study involves computing orbital ephemerides for known transiting and radial velocity planets, taking Keplerian orbital elements into account. Analytical expressions for angular star–planet separation as a function of the true anomaly are provided, including the locations of minimum and maximum.
2：Sample Selection and Data Sources:
Data regarding exoplanets and orbital parameters are sourced from the NASA Exoplanet Archive.
3：List of Experimental Equipment and Materials:
Not explicitly mentioned in the abstract.
4：Experimental Procedures and Operational Workflow:
The methodology involves using Keplerian orbital elements and their uncertainties with multiples of the orbital period to calculate epochs of specific orbit locations relative to times of measured periastron passage.
5：Data Analysis Methods:
Analytical expressions are used to calculate uncertainties for maximum angular separation as a function of time for the known exoplanets.
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