中大及其他天文台

  • 鹿林天文台空拍
  • 鹿林天文台一米望遠鏡
    一米望遠鏡控制室
  • 鹿林天文台一米望遠鏡
  • 中大天文台(科一館)
  • 兩米望遠鏡
  • 兩米望遠鏡
  • GROWTH
  • Credit: LSST
  • Credit: LSST

Recent Research + more

  • The team led by Prof. Pan investigated the relation between SN Ia ejecta velocity and their host-galaxy environment, and found that there could exist a relationship between the two parameters. This study focused on the local environmental properties of SNe Ia and revealed possible trend that high-velocity SNe Ia tend to be associated with old stellar populations, while normal-velocity SNe Ia can be found in both old and young stellar populations. This result implies that the normal SNe Ia are likely produced by more than one channel, challenging the previous consensus that they are associated with a single and uniform population. This work has been published in Lin & Pan et al., 2024, MNRAS, 531, 1988

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  • Virgo III is a newly discovered ultra-faint dwarf (UFD) galaxy. We used the Lulin One-meter Telescope (LOT) to search for RR Lyrae associated with this UFD.With deep exposures of LOT that can reach to r~23 mag, we discovered three RR Lyrae, labeled as V1, V2, and V3 in this deep LOT images. Using the discovered RR Lyrae, we measured a distance of 154 kpc to Virgo III.

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  • An international team led by Prof. Pan studied the data obtained from Pan-STARRS1 Medium Deep Survey (PS1-MDS) and found the type Ia supernovae (SNe Ia) could evolve with time. As one of the most mature cosmological probes, SNe Ia have homogeneous properties, and they were expected to be consistent and similar during the evolution of our Universe. However, this work suggests that SNe Ia are likely to have at least two different populations, as separated by their ejecta velocities. The fractions between different populations tend to evolve with time. This result could impact the precision of SNe Ia in probing the cosmic expansion and dark energy. This work has been published in Pan et al., 2024, MNRAS, 532, 1887 .

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  • Caption: Temporal mass accretion rates during unstable accretion bursts. The upper panel shows DL Tau, and the lower panel shows Haro 6-13. The left side of the figure displays the simultaneous accretion luminosity bursts observed by TESS, ZTF, or ASAS-SN. The horizontal axis represents time (in days), and the vertical axis represents normalized flux. The right side of the figure presents the derived temporal mass accretion rates. The horizontal axis represents time (in days), and the left vertical axis (black) represents accretion rates (in units of M☉/yr), while the right vertical axis (blue) represents accretion luminosity (in units of erg/s).

    PhD student Chia-Lung Lin: We have combined photometric and spectroscopic surveys from both space telescopes (TESS) and ground-based telescope (LAMOST, ZTF, and ASAS-SN) to study the mass accretion rates, flare activities, and variability characteristics of 16 Classical T Tauri Stars (CTTS) in Taurus. By calculating the flux of various spectral lines such as H-alpha, we derived an average mass accretion rate of 1.76×10-9 M☉/yr for these 16 CTTSs. Among them, two stars, DL Tau and Haro 6-13, exhibited temporary brightness increases in their TESS light curves due to bursts of unstable mass accretion rates. By analyzing simultaneous monitoring data from ZTF, ASAS-SN, and TESS, we estimated the time series variations in mass accretion rates for these two stars over a span of 50 days. If the results from spectral data reflect a stable accretion pattern, we concluded that the mass accretion behavior of these two stars is primarily driven by stable accretion. Additionally, we detected a total of 13 large flares across these 16 stars, with energy ranging from 2×1034 to 6×1035 erg, making their flare activity more than a hundred times more active than that of solar-like stars. We also found that the variability classes of these 16 stars change over time, with the timescales of these changes falling roughly between 1.6 to 4 years compared to results in the literature.

    This study has been published in Astronomical Journal in 2023, August: Lin, C.-L., Ip, W.-H., Hsiao, Y., et al. 2023, AJ, 166, 82 (Including Prof. Ip, Wing-Huen, master graduate Hsiao, Yao and Cheng, Tzu-Hueng in the IANCU)
    DOI: 10.3847/1538-3881/ace322

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  • Master student Yao-Wen Jhang and Prof. Yi Chou report the analysis results of X-ray light curves collected by Neutron star Interior Composition ExploreR (NICER) from June 2017 to July 2022 of the X-ray binary 4U 1820-30, located at the globular cluster NGC 6624. From the yearly orbital phases obtained by the orbital modulation light curves and historical records, we measured that the observed orbital period derivative is 1/P dP/dt = (-5.21±0.13)×10-8 yr-1 from a time span of 46.3 years database. No significant second order orbital period derivative can be found with 2σ upper limit of | d2P / dt2 | < 5.48×10-22s s-1. To explain the complete different orbital period evolution trends from theoretical prediction and observation result, we agreed that it is caused by the acceleration of the binary system in the gravitational field of globular cluster NGC 6624, as suggested by previous studies. However, we pointed out that it is improper to estimate the acceleration of 4U 1820-30 by observed orbital period derivative because there are too much uncertainties in the intrinsic orbital period derivative. Furthermore, we detected a modulation with a period of 691.6±0.7 s in the NICER X-ray light curves, which is consistent with the superhump period discovered in the far-ultraviolet band of Hubble Space Telescope. In addition to explaining how the superhump modulation can be detected in X-ray band, we also suggested that this periodic modulation may be induced by a hierarchical third star that orbits around the binary system. These results have been published in Chou & Jhang 2023 ApJ, 951, 42.

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  • Based on light curves data taken from ZTF and published distances, the team led by Prof. Chow-Choong Ngeow derived the gri-band period-luminosity (PL) relations for various types of pulsating stars located in the globular clusters. These include RR Lyrae, Type II Cepheids, and anomalous Cepheids. Many of these PL relations were derived for the first-time in gri filters, with potential applications in the era of Rubin Observatory’s LSST. These works are published in Ngeow et al (2022, AJ 163:239, AJ 164:154, and AJ 164:191).

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Honor+ more

  • 恭賀本所陳婷琬助理教授榮獲113年新聘教研人員獎勵。 (2024-07-04)
  • 恭賀 本所碩士班吳君磊同學獲得 112學年度第2學期國立中央大學優秀學生獎學金 (2024-05-03)
  • 恭喜 碩士班一年級吳君磊同學榮獲本所112年度第一學期學業優秀獎學金 (2024-03-20)
  • 恭喜 本所葉永烜教授榮獲本校113年度國鼎獎座教師、高仲明教授榮獲本校113年度特聘教授、本所饒兆聰教授榮獲本校113年度研究傑出獎 (2024-03-08)
  • 恭賀 本所博士班謝天葦(Tanvi Sharma)獲2024年物理年會壁報佳作獎 (2024-01-29)

Academic Event

  • No Meeting & Workshop

Colloquium

  • Date: 2024-08-06
  • Time: 14:00
  • Location: S4-1013
  • Speaker: Prof. Hua-Bai Li
  • Title: A Unified Interpretation of Magnetic Field and Turbulence Observations

Journal Club

  • 近期無期刊導讀

    • Visiting Scholar + more

    • Dr. Li-Chiang Huang (2024-05-01~2024-08-31)