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Activity > Lunch Talk

Lunch Talk (2021)

ASIAA Lunch Talk is an institute-wide event allowing ASIAA researchers from different fields to discuss astronomy in a very casual manner. The informal meeting is usually held at lunch time on every Monday. Occasionally visitors are also invited to the lunch talk to share their research and ideas with ASIAA researchers.

    Contact
  • Lunch Talk: Colloquium Committee (talks_replace2@_asiaa.sinica.edu.tw)
  • Tech Lunch Talk: Chang, Hsiao-Wen (hwchang_replace2@_asiaa.sinica.edu.tw)
NEXT Lunch Talk: 2021-04-26 Mon 12:15~13:15 [R1203]
Speaker:TC Chen, MK Lin, N Hirano, O Yoichi, WH Wang, H Hirashita
Topic:Faculty Presentation I.
No. Time/Place Speaker Topic (Abstract)
download PDF: dowaload talk PDF file
12021-06-28 Mon
12:00~13:00
12F open area
[Pizza lunch] Ryu Makiya
[ASIAA]
22021-05-24 Mon
12:15~13:15
R1203
YW Tang, YH Chu, LY Chiang, CF Lee, MT Chen, SY Wang
[ASIAA]
Faculty Presentation V
32021-05-17 Mon
12:15~13:15
R1203
YT Lin, PG Gu, S Matsushita,H Shang, N Ohashi, K Umetsu
[ASIAA]
Faculty Presentation IV
42021-05-12 Wed
12:05~13:00
R1203
Chang, Hsiao-Wen
[ASIAA]
52021-05-10 Mon
12:15~13:15
R1203
HW Yen, LH Lin, YJ Hwang, SY Liu, T Okumura, K Asada
[ASIAA]
Faculty Presentation III
62021-05-03 Mon
12:15~13:15
R1203
KJ Chen, P Koch, HY Liu, K Sakamoto, MJ Wang, M Takami
[ASIAA]
Faculty Presentation II
72021-04-28 Wed
12:05~13:00
R1203
Lu, Lou-Chien
[ASIAA]
82021-04-26 Mon
12:15~13:15
R1203
TC Chen, MK Lin, N Hirano, O Yoichi, WH Wang, H Hirashita
[ASIAA]
Faculty Presentation I.
92021-04-14 Wed
12:05~13:00
R1203
Chen, Pai-An
[ASIAA]
3D列印的操作簡介與應用
102021-03-31 Wed
12:05~13:00
R1203
Zhong, Jie-Ying
[ASIAA]
Millimeter Wave Transceiver Components for 5G Application.
112021-03-22 Mon
12:00~13:00
R1203
[Pizza lunch] Marius Lehmann
[ASIAA]
Density Waves in Saturn's Rings
Abstract

I will briefly discuss the occurrence and detection of spiral density waves and the viscous overstability in Saturn's rings. The former typically being excited by moons orbiting outside the rings, with typical wavelengths of some tens of kilometers, the latter being a spontaneous instability of the ring flow, instigating axisymmetric density wave trains on a 100m scale. The study of these wave structures can provide insights in principles of disk-satellite interaction and disk dynamics, and is therefore of fundamental interest for astrophysical disks. For instance, the actions of moons that orbit interior and exterior to Saturn’s rings bear many similar- ities to those of planets forming in proto-planetary disks. Furthermore, by utilizing a fluid description of the rings, the analysis of these wave structures in Saturn’s rings can provide important physical pa- rameters which are otherwise hard to constrain, such as the local mass surface density and the viscosity of the rings.

122021-03-17 Wed
12:05~13:00
R1203
Martin-Cocher, Pierre
[ASIAA]
The Menerga HVAC: the system for regulating the temperature in GLT receiver cabin.
132021-03-03 Wed
12:05~13:00
R1203
Yen, Wei-Ling
[ASIAA]
深入淺出css.
142021-02-17 Wed
12:05~13:00
R1203
Ma Del Carmen Ayala Loera
[ASIAA]
Photometric studies of TransNeptunian objects, colours and surface characterization.
152021-02-03 Wed
12:00~13:00
R1203
Chiu, Chuang Ping
[ASIAA]
The calibration source design and analysis.
162021-01-25 Mon
12:15~13:15
R1203
Cheng-Han Hsieh
[Yale University]
Evidence that 'Oumuamua is the ~45Myr-old product of a Molecular Cloud
Abstract

The arrival of ISOs -- and specifically the appearance of 1I/'Oumuamua -- points to a significant number density of free-floating bodies in the Solar neighborhood. We study the details of 'Oumuamua's pre-encounter galactic orbit and find that it encountered our Sun at very nearly its maximum vertical and radial excursion relative to the galactic plane. 'Oumuamua's kinematics, moreover, strongly resemble those of nearby Young Associations. To obtain an order-of-magnitude a-priori age estimate, we compared 'Oumuamua's orbit to the orbits of 13,066 F-type stars drawn from the Gaia DR2, and with a simple diffusion model, we find tau_`O ~35 Myr. We then compare 'Oumuamua's orbit with the trajectories of nearby moving groups, confirming that its motion is consistent with its membership in the Carina and Columba associations, whose ages are 45 Myr. We conducted Monte Carlo simulations that trace the orbits of test particles ejected from the stars in the Carina and Columba associations. We find that to achieve the inferred Pan-STARRS number density of 0.2 ISOs per au^3, the required ejection mass is ~ 100 M_{Jup} per known star within the associations. The Pan-STARRS observation is thus in significant tension with scenarios that posit 'Oumuamua's formation and ejection from a protostellar disk.

172021-01-20 Wed
12:00~13:00
R1203
Chen, Ying-Tung
[ASIAA]
現代克卜勒 - 運用現代天文學創造更多的能源
182021-01-18 Mon
12:15~13:15
R1203
Yuji Matsumoto
[ASIAA]
Formation of multiple-planet systems in resonant chains around M dwarfs
Abstract

Recent observations have revealed the existence of multiple-planet systems composed of the Earth-mass planets around late M dwarfs. Planets around late M dwarfs tend to be in or near resonant chains, while those around FGK dwarfs are not. We investigate the formation of multiple-planet systems in resonant chains around low-mass stars. A time-evolution model of the multiple-planet formation via pebble accretion in the early phase of the disk evolution is constructed based on the formation model for the TRAPPIST-1 system. We find that there is a range of the protoplanet formation timescale for forming the stable multiple-planet systems in resonant chains. This range depends on the stellar mass. We suggest that the protoplanet formation timescale is a key parameter for the formation of multiple-planet systems with planets in resonant chains around low-mass stars.

192021-01-11 Mon
12:15~13:15
R1203
James Hung-Hsu Chan
[ASIAA]
Measuring accretion disk sizes of lensed quasars with microlensing time delay in multi-band light curves
Abstract

I will present a new method to measure the color-dependent source size in lensed quasars using the microlensing time delays inferred from multi-band light curves. In practice, the relevant observable is the differential microlensing time delays between different bands. I will show from simulation using the facility as Vera C. Rubin Observatory that if this differential time delay between bands can be measured with a precision of 0.1 days in any given lensed image, the disk size can be recovered to within a factor of 2. If four lensed images are used, our method is able to achieve an unbiased source measurement within the error of the order of 20%, which is comparable with other techniques.

202021-01-06 Wed
12:00~13:00
R1203
Huang, Pin Jie
[ASIAA]
Subaru 望遠鏡:MCS 主鏡調整機構說明
TEL: 886-2-3365-2200 FAX: 886-2-2367-7849
General: asiaa_replace2@_asiaa.sinica.edu.tw Media Request: epo_replace2@_asiaa.sinica.edu.tw
11F of AS/NTU Astronomy-Mathematics Building, No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan, R.O.C.