• The Bulletin of The Korean Astronomical Society
• /
• v.44 no.2
• /
• pp.72.1-72.1
• /
• 2019

Symbiotic stars are wide binary systems of a white dwarf and a mass losing giant, exhibiting various activities mainly attributed to accretion of a fraction of slow stellar wind emanating from the giant. We perform 3 dimensional hydrodynamical simulations using the FLASH code to investigate the formation and physical structures of an accretion disk in symbiotic stars with binary separation in the range of 2-4 au. Radiative cooling is introduced in the flow in order to avoid acute pressure increase in the vicinity of the accretor that may prevent stable disk formation. By setting the same density condition in front of the bow shock generated in two different velocity fields, the role of ram pressure balancing between the disk and the wind is examined. We find that three main streams (direct stream from the giant, stream following the accretion wake, and stream passing through the bow shock front) all feed the disk, and their individual contributions on the mass accretion onto the white dwarf are explored.

• The Bulletin of The Korean Astronomical Society
• /
• v.44 no.2
• /
• pp.60.3-60.3
• /
• 2019

Binary systems of a white dwarf showing mass transfer activities are classified into cataclysmic variables and symbiotic stars. In the case of cataclysmic variables, the companion is usually a late type main sequence star filling its Roche lobe, where material is transferred through the inner Lagrangian point to form an accretion disk around the white dwarf. The disk becomes unstable and highly viscous when the surface density exceeds the critical density, leading to dwarf nova outbursts. In contrast, symbiotic stars are wide binary systems having a giant as the mass donor. Some fraction of giant stellar wind is accreted to the white dwarf giving rise to various symbiotic activities. In particular, half of symbiotics show Raman O VI at 6830 and 7088, which are important spectroscopic probe of mass transfer process. Monitoring observations using 1 m class telescopes will produce valuable information regarding the mass loss and mass transfer to white dwarf stars, shedding much light on the last stage of stellar evolution of low and intermediate mass stars.

• Animal cells and systems
• /
• v.5 no.4
• /
• pp.291-297
• /
• 2001

Three species of endosymbiotic dinoflagellates, zooxanthellae, are investigated from six host species of anthozoans from Korea. Three unrecorded endosymbionts species are Symbiodinium kawagutii, Symbiodinium microadriaticum, and Symbiodinium sp. Symbiodinium kawagutii Is associated with Alveopora japonica, Anthopleura japonica and Parasicyonis actinostoloides. Symbiodinium microadiraticum is found in Anthopleura kurogane and Parasicyonis sp. Unlike the former two symbionts, Symbiodinium sp. is associated with Anthopleura midori.

• The Bulletin of The Korean Astronomical Society
• /
• v.36 no.2
• /
• pp.148.2-148.2
• /
• 2011

Many symbiotic stars exhibit features formed through Raman scattering with hydrogent atom, which can be useful in probing the mass loss and mass transfer processes. These include Raman scattered O VI 6830, 7088, Raman scattered He II 6545, 4850, 4332, and broad wings around Balmer emission lines. In this study we investigate the basic properties of broad Balmer wings formed through Raman scattering using a Monte Carlo technique. Special attention is made on the symmetry of the wings which is expected to be broken due to asymmetric scattering cross section. In this poster, we show preliminary results.

• Proceedings of the Botanical Society of Korea Conference
• /
• 1987.07a
• /
• pp.81-101
• /
• 1987

In an attempt to revies the informations about genes involved in symbiotic nitrogen fixation, developmental processes in which host plant interact with microbe during nodule formation were introduced first. The structure, function and regulation of the genes discussed were mainly about microbial genes; those involved in the process of nodule formation (nod-genes) and of nitrogen fixation (nif-genes). Informations about the host genes involved in the symbiosis were discussed briefly.

• Journal of Electrical Engineering and Technology
• /
• v.11 no.5
• /
• pp.1210-1215
• /
• 2016

• Applied Chemistry for Engineering
• /
• v.27 no.1
• /
• pp.1-9
• /
• 2016

The co-culture system of microalgae and bacteria enables simultaneous removal of BOD and nutrients in a single reactor if the pair of microorganisms is symbiotic. In this case, nutrients are converted to biomass constituents of microalgae. This review highlights the importance and recent researches using symbiotic co-culture system of microalgae and bacteria in wastewater treatment, focusing on the removal of nitrogen and phosphorus. During wastewater treatment, the microalgae produces molecular oxygen through photosynthesis, which can be used as an electron acceptor by aerobic bacteria to degrade organic pollutants. The released $CO_2$ during the bacterial mineralization can then be consumed by microalgae as a carbon source in photosynthesis. Microalgae and bacteria in the co-culture system could cooperate or compete each other for resources. In the context of wastewater treatment, positive relationships are prerequisite to accomplish the sustainable removal of nutrients. Therefore, the selection of compatible species is very important if the co-culture has to be utilized in wastewater treatment.

• The Bulletin of The Korean Astronomical Society
• /
• v.41 no.2
• /
• pp.57.3-58
• /
• 2016

A symbiotic star is a wide binary system consisting of a hot white dwarf and a mass losing giant, where the giant loses its material in the form of a slow stellar wind resulting in accretion onto the white dwarf through gravitational capture. Symbiotic stars are known to exhibit unique spectral features at 6825 and 7082, which are formed from O VI 1032 and 1038 through Raman scattering with atomic hydrogen. In this Monte Carlo study we investigate the flux ratio of 6825 and 7082 in a neutral region with a geometric shape of a slab, cylinder and sphere. By varying the amount of neutral hydrogen parametrized by the column density along a specified direction, we compute and compare the flux ratio of Raman scattered O VI 6825 and 7082. In the column density around 1020 cm-2, flux ratio changes in a complicated way, rapidly decreasing from the optically thin limit to unity the optically thick limit as the column density increases. It is also notable that when the neutral region is of a slab shape with the O VI source outside the slab, the optically thick limit is less than unity, implying a significant fraction of O VI photons escape through Rayleigh scattering near the boundary. We compare our high resolution CFHT data of HM Sge and AG Dra with the data simulated with finite cylinder models confirming that 'S' type symbiotic tend to be characterized by thicker HI region that 'D' type counterparts. It is expected that this study will be useful in interpretation of the clear disparity of Raman O VI 6825 and 7082 profiles, which will shed much light on the kinematics and the asymmetric distribution of O VI material around the hot white dwarf.

• Journal of The Korean Astronomical Society
• /
• v.36 no.2
• /
• pp.55-60
• /
• 2003

In Lee, Kang & Byun (2001) the discovery of Raman scattered 6545 A feature was reported in symbiotic stars and the planetary nebula M2-9. The broad emission feature around 6545 A is formed as a result of Raman scattering of He II n = 6 $\to$ n = 2 photons by atomic hydrogen. In this paper, we introduce a method to compute the equivalent width of He II $\lambda$ 1025 line and present an optical spectrum of the symbiotic star RR Telescopii as an example for a detailed illustration. In this spectrum, we pay attention to the broad H$\alpha$ wings and the Raman scattered He II 6545 feature. The broad Ha wings are also proposed to be formed through Raman scattering of continuum around Ly$\beta$ by Lee (2000), and therefore we propose that the equivalent width of the He II $\lambda$ 1025 emission line is obtained by a simple comparison of the strengths of the 6545 feature and the broad H$\alpha$ wings. We prepare a template H$\alpha$ wing profile from continuum radiation around Ly$\beta$ with the neutral scattering region that is supposed to be responsible for the formation of Raman scattered He II 6545 feature. Isolation of the 6545 feature that is blended with [N II] $\lambda$ 6548 is made by using the fact that [N II] $\lambda$ 6584 is always 3 times stronger than [N II] $\lambda$ 6548. We also fit the 6545 feature by a Gaussian which has a width 6.4 times that of the He II $\lambda$ 6527 line. A direct comparison of these two features for RR Tel yields the equivalent width $EW_{Hel025} = 2.3{\AA}$ of He II $\lambda$ 1025 line. Even though this far UV emission line is not directly observable due to heavy interstellar extinction, nearby He II lines such as He II $\lambda$ 1085 line may be observed using far UV space instruments, which will verify this calculation and hence the origins of various features occurring in spectra around H$\alpha$.

• Journal of the Korean earth science society
• /
• v.38 no.1
• /
• pp.1-10
• /
• 2017

The symbiotic star AG Peg is a nebulous binary system that consists of giant star (GS) and white dwarf (WD). We investigated the HI Balmer emission lines of the symbiotic nova AG Peg, observed in 1998, 2001, and 2002 at Lick Observatory. The $H{\alpha}$ and $H{\beta}$ line profiles consist of blue-shifted, red-shifted, and broad components of which intensities and width showed notable changes. The HI emission line profiles that represent the kinematics of the gaseous nebula appear to be mainly from an accretion disk in relatively large radius from the WD. Considering the line of an observer's sight, both GS and WD are located at the sky plane side by side during the 1998 observation, while the WD is in front of GS during 2002 but the WD in rear during 2001. Such a relative position and the spectral line intensity variation imply that a fairly constant outflow occurs into WD from GS which caused to maintain the rotating thick accretion disk structure responsible for the observed spectral lines.