• 천문학회보
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• 제40권1호
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• pp.69.1-69.1
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• 2015

Classical T Tauri star DG Tau is suggested as the driving source of parsec-scale jet which expands up to 650" (0.4 pc). To investigate the kinematics and physical properties of the jet, we have obtained the optical emission lines of $H{\alpha}$, [O I] ${\lambda}{\lambda}$6300, 6363, [N II] ${\lambda}{\lambda}$6548,6584, and [S II] ${\lambda}{\lambda}$6716, 6731 from HH 158 ad HH 702. The radial velocity of HH 158 is in the range of -50 to $-250km\;s^{-1}$. For HH 702, located at 650" from the source, it shows ~ $-80km\;s^{-1}$. In HH 158, the electron density ($n_e$) close to the star is ${\sim}10^4cm^{-3}$ and it decreases to ${\sim}10^2cm^{-3}$ at 14" away from the star. Electron temperature ($T_e$) is decreasing from >15,000 K to ~5,000 K with distance. Ionization fraction ($x_e$) is increasing from almost zero to > 0.4 along the distance. In HH 702, the values of $n_e$, $T_e$, and $x_e$ are similar to those estimated at 14" from source, where knot C of HH 158 is located. This may imply that the physical properties of the knot could persist through such a long distance in the space, and the gas could be re-excited by the shock during propagation of the jet. On the other hand, we cannot avoid the possibility that HH 702 is driven by another source rather than DG Tau because HH 158 and HH 702 show somewhat large difference in their inclination angles (${\Delta}i=21-35^{\circ}$).

• 천문학회지
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• 제38권2호
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• pp.249-252
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• 2005

We present results of the velocity-resolved spectroscopy of the [Fe II] $\lambda$1.644${\mu}m$ emission toward outflow sources with the Subaru Telescope at the angular resolution of 0.apos;16 ${\~}$ 0.apos;5 arcseconds. The observed sources are L1551 IRS 5, DG Tau, HL Tau and RW Aur, which are located in the Taurus-Aurigae Molecular Cloud, one of the closest star forming regions (0.apos;1 = 14 AU). We were able to resolve outflow structure in the vicinity of the sources at a scale of a few tens of AU. The position-velocity diagram of each object shows two velocity components: the high velocity component (HVC: 200 - 400 km $s^{-l}$) and the low velocity component (LVC: 50 - 150 km $s^{-l}$), which are clearly distinct in space and velocity. The HVC may be a highly collimated jet presumed from its narrow velocity width and high velocity. The LVC, on the other hand, may be a widely opened disk wind inferred from its broad velocity width and low velocity. The spectrum taken perpendicular to the L1551 IRS 5 outflow at its base shows that the LVC has a spatially wide subcomponent, supporting the above interpretation. We demonstrated that the [Fe II] 1.644 $\mu$ spectroscopy is a very powerful tool for the studies of fast jets and winds that directly emanate from star-disk systems.

• 천문학회보
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• 제40권1호
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• pp.81.2-81.2
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• 2015

FU Orionis 형 천체는 태양 질량의 2배 이하인 T Tauri 별 중에서도 급격한 밝기 변화를 보이는 별들로서, 광도 증가폭이 최대 5등급에 이르는 것으로 알려져 있다. 이러한 현상의 원인은 FU Orionis를 둘러싼 강착 원반에서 나타나는 불안정성에 의해, 원반 안쪽의 물질이 한꺼번에 중심별로 쏟아져 내리기 때문인 것으로 분석된다. V1057 Cyg는 FU Orionis 형 천체 중 하나로, 1969년에 급격한 밝기 변화를 일으키며, 기존의 16등급에서 변화 직후 9등급 후반에 이르는 광도 증가를 보였다. 우리는 V, R, I 필터 대역에서 관측을 수행하였으며, 본 발표에서는 2013 ~ 2014년에 걸쳐 소백산, 레몬산 천문대 및 경희천문대에서 관측한 결과를 보고한다.

• 천문학회보
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• 제40권2호
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• pp.36.1-36.1
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• 2015

We present $5-14{\mu}m$ Infrared Spectrograph spectra of 14 T Tauri stars which show Polycyclic Aromatic Hydrocarbon (PAH) features and reside in 0.7 pc from ${\Theta}_1$ Ori C. The spectral types of nine out of 11 stars have spectral type information, with types ranging from K7-M5. These stars do not supply strong enough UV photons to excite PAH emission in their disks. Therefore, we consider the detection of PAH emission in disks around low mass stars illuminated by an external source of UV photons, namely, from Trapezium OB association, including ${\Theta}_1$ Ori C. The morphological features of PAH emission from most disks around K-M type host stars are unique, not belonging to any known classes of PAH features. We found that the PAH emission strengths decrease as the projected distance of the objects from ${\Theta}_1$ Ori C increase. We suggest future far-IR and submm/mm observations for better understanding of the characteristics and distribution of PAHs in these disks.

• 천문학회보
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• 제38권1호
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• pp.54.2-54.2
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• 2013

FUors are believed in the outburst phase of the episodic accretion model with accretion mass rates enhanced by 2-3 orders of magnitude compared to the normal classical T-Tauri stars. We have been monitoring HBC 722, which was brightened by ~5 mag in the V band in 2010 and thus became a new FUor, with BOES. We also observed two other FUors, FU Ori and V1057 Cyg with BOES. V1057 Cyg has been monitored in the optical spectroscopy for decades since its outburst. We present the results of our 2-year monitoring observations of HBC 722 in comparison with FU Ori and V1057 Cyg.

• 천문학회보
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• 제39권1호
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• pp.63.1-63.1
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• 2014

We present a study on the parsec-scale jets from young stellar objects using long-slit spectroscopic data obtained from Bohyunsan Optical Astronomy Observatory on 2012 - 2014. Through the position-velocity diagrams, we show the radial velocity variation, peak velocity and velocity width of the outflow from several T Tauri stars and Herbig Ae/Be star. $H{\alpha}$, [OI] 6300/6363, [NII] 6548/6584 and [SII] 6716/6731 emission lines are obtained and they show various velocity features. We also compare our result with other data from literatures.

• 천문학논총
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• 제15권spc1호
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• pp.93-102
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• 2000

We have reviewed the magnetic activity in close binaries. Solar like magnetic activity indicators such as photometric spots, chromo spheric emission, coronal X-ray and radio emission, and flare activity are commonplace in many cool stars with convective envelopes. Using the UV spectra we confirmed the strength of stellar activity increases with more rapid rotation and later spectral types which corresponds to the increasing depth of the star's convective envelope. Apart from very young stellar objects such as T Tauri stars, the stars with the highest levels of activity are close binary systems composed of cool stars, i.e., the chromospherically active binaries such as RS CVn, BY Dra, W UMa and related systems. The IUE low and high dispersion spectra of V711 Tau, VW Cep and SW Lac are used for ultraviolet photometry and for a variation study of chromospheric activity. Evidence of chromospherically activity is indicated by the intensity variation of the Mg II emission line with orbital phase.

• 천문학회지
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• 제29권2호
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• pp.107-117
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• 1996

We have studied the star forming activities and dust properties of Lynds 1251, a dark cloud located at relatively high galactic latitude. Eleven IRAS point sources identified toward Lynds 1251 are discussed. Estimate of stellar masses, and far-infrared lumnosities of the young stars associated with two prominent IRAS point sources imply that these are T-Tauri stars with masses smaller than $0.3 M_\bigodot$. The low dust temperature of 27 K and low ratio of FIR emission to hydrogen column density are probably due to the lack of internal heating sources. Presumably two low mass young stars do not have enough energy to heat up the dust and gas associated. The dust heating is dominated by the interstellar heating source, and the weaker interstellar radiation field can explain the exceptionally low dust temperatures found in Lynds 1251. The estimated dust mass of Lynds 1251 is just $\~1M_\bigodot$, or about 1/1000 of gas mass, which implies that there must be a substantial amount of colder dust. The infrared flux at $100{\mu}m$ is matching well with $^{13}CO$ peak temperature, while the $^{12}CO$ integrated intensity is matching with the boundary of dust emission. Overall, the dust properties of Lynds 1251 is similar to those of normal dark clouds even though it does have star forming activities.

• 천문학회지
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• 제56권2호
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• pp.253-262
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• 2023

This work presents four high-amplitude variable YSOs (≃3 mag at near- or mid-IR wavelengths) arising from the SPICY catalog. Three outbursts show a duration that is longer than 1 year, and are still ongoing. And additional YSO brightened over the last two epochs of NEOWISE observations and the duration of the outburst is thus unclear. Analysis of the spectra of the four sources confirms them as new members of the eruptive variable class. We find two YSOs that can be firmly classified as bona fide FUors and one object that falls in the V1647 Ori-like class. Given the uncertainty in the duration of its outburst, an additional YSO can only be classified as a candidate FUor. Continued monitoring and follow-up of these particular sources is important to better understand the accretion process of YSOs.

• 천문학회보
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• 제41권1호
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• pp.60.1-60.1
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• 2016

태양과 같은 별의 형성기작은 질량이 큰 별의 형성기작에 비해 비교적 잘 연구되어 왔다고는 하지만, 이 또한 온전한 이해와는 거리가 먼 상황이며 여전히 논란의 대상이다. IRAS, Spitzer와 같은 적외선우주망원경으로 얻어진 원시성의 광도함수는 일반적으로 받아들여졌던 별탄생 이론으로 설명되지 못한다는 것이 밝혀졌고, 이에 새로운 별탄생 이론이 필요하게 되었다. 새롭게 받아들여지고 있는 별탄생 모델은 Episodic Accretion 모델로서, 원시행성계원반에서 원시성으로 질량 강착이 간헐적이면서 폭발적으로 일어난다는 것이다. 이러한 모델의 관측적 증거의 하나는 FU Orionis와 같은 천체로서, T-Tauri 단계에 있는 원시성이 본래의 밝기보다 약 100배, 즉 가시광에서 5등급 이상 폭발적으로 밝아진 천체이다. 질량강착의 과정은 행성형성의 초기조건을 결정하는 원시행성계원반의 물리적, 화학적 특성을 결정하므로, 그 이해가 중요하다. 따라서 본 연구팀은 Episodic Accretion이 원시행성계원반과 원시항성풍의 형성과 진화에 어떤 역할을 하는지 연구하기 위하여, 보현산 천문대의 고분산 분광기인 BOES를 이용하여, 최근에 폭발을 일으킨 원시성인 HBC 722와 2MASS J06593158-0405277을 모니터링 관측을 해왔으며, 이전에 알려진 6개의 FU Orionis 형 천체들도 관측하였다. 여기서는 그 결과를 발표하고자 한다.