| dc.description.abstract | The main-belt asteroids provide valuable information for us to study the general history of the solar system since they are considered the leftover planetesimals during the formation and evolution of the planetary disk. In order to understand the role-play of asteroids in planetary system formation, tracing the physical parameters to figure out the actual structures and compositions is one important way. We aim to investigate the albedo, which is related to the composition and structure of asteroids, by multi-method such as 1)polarimetry using the Triple Range Imager and Polarimeter (TRIPOL) instrument, 2) photometry of Charge-coupled device (CCD) instrument, and 3) a spectrum of LISA spectrograph, observations on the Lulin One-meter Telescope (LOT).
In the first part of this thesis, we demonstrated the technical properties and capability of TRIPOL instrument. We observed a number of bright asteroids with known taxonomic classifications at different phase angles, including B-type, C-type, Ch-type, M-type, S-type, and L-type. By measuring polarization degree with phase angle tracing, We confirmed the validity and reliability of the TRIPOL instrument were working. Furthermore, to study the surface texture of a single asteroid, we also measured rotationally resolved photo-polarimetric variation of a metal-rich object (16) Psyche. Our measurements showed no change in the $g′$-$r′$ and $r′$-$i′$ colors of the rotationally resolved photometry and the intriguing variability in the polarization degree as a function of the rotational phase. The TRIPOL instrument can also be used to measure the polarization of the Barbarians with higher phase angles.
In the second part of this thesis, utilizing the Lightcurve database, NEOWISE, and Hierarchical Clustering Method (HCM) datasets, we analyzed to investigate the differences in size, shape, and rotation period distributions among two S-type and C-type asteroid families based on the compositions and the rubble-pile structure model. From the rotation period distributions, we found that the S-type and C-type asteroids have different spin limits, with the S-type period P$_s$ = 2 hours and the C-type period P$_c$ = 3 hours, respectively. That implies the difference in their bulk densities. In addition, we analyzed a sizable C-type super-fast rotator candidate, asteroid (3599) Basov, to look into the rotation period and taxonomic classification through photometry and spectroscopy using the Lulin One-meter Telescope (LOT) at the Lulin Observatory. The rotation period of asterid (3599) Basov was 2.157$pm0.037$ hours, and the result of reflectance spectrum result was similar to typical C-type asteroids. | en_US |