JOVIAN AND EXOPLANET AURORAL RADIO EMISSION PROFILE IN THE LOW-FREQUENCY RANGE

• Main Author: Andary Soraya, Nabila
• Format: Final Project
• Language: Indonesia
• Subjects: Astronomi
• Online Access: https://digilib.itb.ac.id/gdl/view/60917
• Institution: Institut Teknologi Bandung

Earth and giant planets in our Solar System are known to possess an internal magnetic eld and a thick atmosphere that are capable of producing non- thermal low-frequency radio emissions through the Cyclotron Maser Instabili- ty (CMI) mechanism. Particularly for Jupiter, interactions with its satellites can also in uence the probability of detecting radio emissions. In line wi- th this analogy, such radio emissions are expected to be detected from other exoplanetary systems, especially Jupiter-like exoplanets. This thesis focuses on planetary radio emissions in our Solar System and how its detection me- chanism can be applied for exoplanetary systems. It is also expected to give informations about the physical properties of exoplanets, not limited to only conrming its existence. Using ExPRES (Exoplanetary and Planetary Radio Emission Simulator) code, we explain how and what are the physical properties of an exoplanet system that can be inferred from observed dynamic spectra based on previ- ously made assumptions of the radio emission source(s). Simulated dynamic spectra from ExPRES show incredibly well conformity with observational da- ta from Nancay Decameter Array (NDA), Voyager 1 & 2, and Juno that have been carried before, so it is considered applicable for exoplanetary studies and detections. We show and analyze the shape and temporal modulations from si- mulated dynamic spectra to draw out physical information of the exoplanetary system through radio observations. This information includes magnetic eld strength, orbital inclination, rotational and orbital periods, and the magnetic eld tilt and oset. This approach is expected to be a proper framework for future detections of radio emissions from exoplanetary systems.