• The Bulletin of The Korean Astronomical Society
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• v.35 no.2
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• pp.77.1-77.1
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• 2010

One ingredient in an empirical birthrate estimate for pulsar binaries is the fraction of sky subtended by the pulsar beam: the pulsar beaming fraction. This fraction depends on both the pulsar's beam geometry defined by the pulsar's opening angle and the misalignment angle between its spin and magnetic axes. The current estimates for pulsar binary birthrates are based on an average value of beaming fractions for only two pulsars, i.e., PSRs B1913+16 and B1534+12. In this work, we revisit the observed pulsar binaries to examine the sensitivity of birthrate predictions to different assumptions regarding the pulsar beam geometry. The results show that, for those pulsars without any direct beam geometry constraints, the estimated beaming correction factor is likely to be smaller than six, a canonically adopted value when calculating birthrates of Galactic pulsar binaries. The median birthrate estimates for pulsar-white dwarf and pulsar-neutron star binaries in the Galactic disk, based on the best observational constraints, are 34 per Myr and 89 per Myr, respectively.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.2
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• pp.79.2-79.2
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• 2014

Galactic radio pulsar population is diverse. So far about 2300 radio pulsars are known in the Milky Way, in addition to Large and Small Magellanic Clouds. Radio pulsar observations at a few hundreds MHz up to ~10 GHz have been active and they are proved to be fruitful. Low frequencies are preferred mainly because of the steep ratio spectrum of pulsars. However, developments in pulsar backends (e.g. a wide-band spectrometer) and improved system sensitivities make it possible to observe pulsars at higher frequencies using large, single-dish telescopes up to ~18 GHz. Going forward, mm-wavelength observations is expected to open a new window in pulsar astronomy. In particular, frequencies well above ~15 GHz are pre-requisite to detect pulsars in the Galactic Center where radio pulsed signals are severely scattered by interactions with the interstellar medium. Recent discoveries strongly imply that there are subsets of pulsars with an apparently flat spectrum, such as magnetars. In April 2014, the first pulsar (magnetar) was discovered only 3 arcmin from Sgr A*, PSR J1745-2900. We will present a brief overview on pulsar populations focusing on those observable at high frequencies. We will also discuss prospects of pulsar observations in mm-wavelengths and how we can utilize the Korean VLBI network.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.1
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• pp.37.1-37.1
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• 2017

We consider a magnetic dipole model of a pulsar and investigate general relativistic effects on electromagnetic radiation from the pulsar. The general relativistic modifications should be found applicable to many well-known issues in pulsar astronomy. Among other things, the modifications of Goldreich-Julian model and subpulse drift would be of significant interest and challenging issues. The electromagnetic fields in the pulsar magnetosphere are computed by solving Maxwell's equations defined in the strongly curved spacetime around the pulsar, hence containing the properties of strong gravitational effects. On top of these effects, we also investigate the effects from rotation and obliqueness of the pulsar to work out the general relativistic versions of Goldreich-Julian model and subpulse drift.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.1
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• pp.78.1-78.1
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• 2014

Pulsar binaries in tight orbits are considered to emit strong gravitational waves (GWs) during the last stage of their coalescences. They form a subset of compact binary mergers, which consists of white dwarfs (WDs), neutron stars (NSs), or black holes (BHs). One of the most famous example of 'merging' pulsar binaries is the Hulse-Taylor pulsar (PSR B1913+16) discovered in 1974 by Russell Hulse and Joseph Taylor. About ten NS-NS and several tens of NS-WD binaries are known in our Galaxy. Merging binaries are rare and only a few NS-NS and NS-WD have been discovered to date. A pulsar with a black hole companion is also theoretically expected, but there is yet no detection. Within several years, direct detections of GWs from compact binary mergers will be made by laser interferometers. This will pave a way to study physics of compact binaries that cannot be reached by electromagnetic waves (EM). Pulsar binaries are of particular interest as we can use both EM and GW to probe these systems. In this talk, we present a brief overview on the Galactic pulsar populations and discuss their implications for GW detection.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.1
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• pp.52.1-52.1
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• 2014

Radio pulsars are highly magnetized, rapidly rotating neutron stars that emit synchrotron radiation along the magnetic axes at their spin frequencies. Traditionally, pulsar observations have been done at low frequencies (MHz up to a few GHz), since radio pulsar spectrum is known to a power-law with a steep negative spectral index. More recently, high-frequency pulsar observations (several GHz and above) have been made as a broadband spectrometer and fast computers became available. High-frequency pulsar observations will provide information on radio emission mechanism of pulsars in the vicinity of the neutron star surface. There is also huge interest from gravitational-wave and astrophysics community to find a pulsar in the center of our Galaxy. The Korean VLBI Network has three 21-m single dishes in the Korean peninsula. Using KVN's lowest observational frequency of 22-GHz, we performed test observations with the KVN targeting a few selected known, bright pulsars. In addition, we have been developing pulsar pipelines that can be utilized with a VLBI facility using Mark-V. We present a brief introduction of radio pulsars and show data obtained with the KVN.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.2
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• pp.43.3-43.3
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• 2018

We develop a model for broadband spectral energy distribution (SED) of Pulsar Wind Nebulae (PWNe). The model assumes that electrons/positrons in the pulsar wind are injected into and stochastically accelerated in the pulsar termination shock. We consider two scenarios: a stationary one-zone case and a time-evolving multi-zone case. In the latter scenario, flow properties in the PWNe (magnetic field, bulk speed) are modeled to vary in time and space. We apply the model to the broadband SED of the pulsar wind nebula 3C 58. From the modeling, we find that a broken power-law injection is required with the maximum electron energy of ~200 TeV.

• Journal of Astronomy and Space Sciences
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• v.33 no.2
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• pp.69-73
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• 2016

We use the non-stationary three dimensional two-layer outer gap model to explain gamma-ray emissions from a pulsar magnetosphere. We found out that for some pulsars like the Geminga pulsar, it was hard to explain emissions above a level of around 1 GeV. We then developed the model into a non-stationary model. In this model we assigned a power-law distribution to one or more of the spectral parameters proposed in the previous model and calculated the weighted phase-averaged spectrum. Though this model is suitable for some pulsars, it still cannot explain the high energy emission of the Geminga pulsar. An Inverse-Compton Scattering component between the primary particles and the radio photons in the outer magnetosphere was introduced into the model, and this component produced a sufficient number of GeV photons in the spectrum of the Geminga pulsar.

• Journal of Astronomy and Space Sciences
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• v.33 no.2
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• pp.93-99
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• 2016

A redback system is a binary system composed of a pulsar and a main sequence star. The inverse Compton (IC) scattering between the stellar soft photons and the relativistic pulsar wind will generate orbital-modulating GeV photons. We look for these IC emissions from redback systems. A multi-wavelength observation of an unassociated gamma-ray source, 3FGL J2039.6-5618, by Salvetti et al. (2015) detected an orbital modulation with a period of 0.2 days in both X-ray and optical cases. They suggested 3FGL J2039.6-5618 to be a new redback candidate. We analyzed the gamma-ray emission of 3FGL J2039.6-5618 using the data from the Fermi large area telescope (Fermi-LAT) and obtained the spectrum in different orbital phases. We propose that the spectrum has orbital dependency and estimate the characteristic energy of the IC emission from the stellar-pulsar wind interaction.

• Fashion & Textile Research Journal
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• v.4 no.4
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• pp.399-404
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• 2002

The purpose of this study was to develop the rain melange fabrics with using the pulsar interlacing unit. The properties of the pulsar interlaced yarns (PI yarn) which were textured with the several texturing conditions were analyzed and compared with the regular interlaced yarn (IT yarn) and with normally composited yarn (CP yarn). The results were as follows : The PI yarn which has the best rain random melange effect could be obtained with following texturing condition; 3 kg/$cm^2$ of interlacing air pressure, 1.6 mm diameter of interlacing nozzle and 500 m/min of yarn speed. When IT yarn was compared with CP yarn, IT yarn had higher denier and tenacity than those of CP yarn and had lower elongation and shrinkage than those of CP yarn.

• The Bulletin of The Korean Astronomical Society
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• v.45 no.1
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• pp.53.2-53.2
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• 2020

We measure X-ray timing and spectral properties of the pulsar PSR J0205+6449. Pulsar's rotation frequency ν = 15.20102357(9) s-1 and its derivative ${\dot{\nu}}=-4.5(1){\times}10^{-11}s^{-2}$ are measured, and the pulsed spectrum of 2-30 keV is model of power law with photon index ��psr = 1.07(16) and F2-30 keV = 7.3(6) × 10-13 erg cm-2 s-1. We use thermal emission models and non-thermal model to fit the pulsar spectrum and measure the surface temperature and luminosity of the pulsar. The surface temperature T∞ = 0.5-0.8 MK and luminosity Lth = 1-5 × 1032 erg s-1 are measure, and this result verifies the previous results known to have low surface temperature and luminosity for the age range of