7 research outputs found
Solar Cycle Variations of p-Mode Frequencies
Observations show that the solar p-mode frequencies change with the solar
cycle. The horizontal-phase-velocity dependence of the relative frequency
change, scaled by mode mass, provides depth information on the perturbation in
the solar interior. We find that the smoothed scaled relative frequency change
varies along the solar cycle for horizontal phase velocities higher than a
critical value, which corresponds to a depth near the base of the convection
zone. This phenomenon suggests that the physical conditions in a region near
the base of the convection zone change with the solar cycle
Optical observations of NEA 3200 Phaethon (1983 TB) during the 2017 apparition
The near-Earth asteroid 3200 Phaethon (1983 TB) is an attractive object not
only from a scientific viewpoint but also because of JAXA's DESTINY+ target.
The rotational lightcurve and spin properties were investigated based on the
data obtained in the ground-based observation campaign of Phaethon. We aim to
refine the lightcurves and shape model of Phaethon using all available
lightcurve datasets obtained via optical observation, as well as our
time-series observation data from the 2017 apparition. Using eight 1-2-m
telescopes and an optical imager, we acquired the optical lightcurves and
derived the spin parameters of Phaethon. We applied the lightcurve inversion
method and SAGE algorithm to deduce the convex and non-convex shape model and
pole orientations. We analysed the optical lightcurve of Phaethon and derived a
synodic and a sidereal rotational period of 3.6039 h, with an axis ratio of a/b
= 1.07. The ecliptic longitude (lambda) and latitude (beta) of the pole
orientation were determined as (308, -52) and (322, -40) via two independent
methods. A non-convex model from the SAGE method, which exhibits a concavity
feature, is also presented.Comment: 14 pages, 4 figures, 1 figure in Appendix A. Accepted for publication
in Astronomy & Astrophysics (A&A
Apophis planetary defense campaign
We describe results of a planetary defense exercise conducted during the close approach to Earth by the near-Earth asteroid (99942) Apophis during 2020 December–2021 March. The planetary defense community has been conducting observational campaigns since 2017 to test the operational readiness of the global planetary defense capabilities. These community-led global exercises were carried out with the support of NASA's Planetary Defense Coordination Office and the International Asteroid Warning Network. The Apophis campaign is the third in our series of planetary defense exercises. The goal of this campaign was to recover, track, and characterize Apophis as a potential impactor to exercise the planetary defense system including observations, hypothetical risk assessment and risk prediction, and hazard communication. Based on the campaign results, we present lessons learned about our ability to observe and model a potential impactor. Data products derived from astrometric observations were available for inclusion in our risk assessment model almost immediately, allowing real-time updates to the impact probability calculation and possible impact locations. An early NEOWISE diameter measurement provided a significant improvement in the uncertainty on the range of hypothetical impact outcomes. The availability of different characterization methods such as photometry, spectroscopy, and radar provided robustness to our ability to assess the potential impact risk
Searching for the Signature of the Magnetic Fields at the Base of the Solar Convection Zone with Solar Cycle Variations of [CLC][ITAL]p[/ITAL][/CLC]-Mode Travel Time
Lifetimes of High-[CLC][ITAL]l[/ITAL][/CLC] Solar [CLC][ITAL]p[/ITAL][/CLC]-Modes from Time-Distance Analysis
Taiwan Automated Telescope Network
A global network of small automated telescopes, the Taiwan Automated Telescope (TAT) network, dedicated to photometric measurements of stellar pulsations, is under construction. Two telescopes have been installed in Teide Observatory, Tenerife, Spain and Maidanak Observatory, Uzbekistan. The third telescope will be installed at Mauna Loa Observatory, Hawaii, USA. Each system uses a 9-cm Maksutov-type telescope. The effective focal length is 225 cm, corresponding to an f-ratio of 25. The field of view is 0.62 degree square. The images are taken with a 16-bit 1024×1024 CCD camera. The telescope is equipped with UBVRI filters. Each telescope is fully automated. The telescope
can be operated either interactively or fully automatically. In the interactive mode, it can be controlled through the Internet. In the fully automatic mode, the telescope operates with preset parameters without any human care, including taking dark frames and flat frames. The network can also be used for studies that require continuous observations for selected objects