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STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 On the contribution of black carbon radiative forcing to the total aerosol radiative forcing over an urban environment Panicker Abhilash 1 , Pandithurai G 1 , Safai P. D 1 , Lee Dong-In 2 , Dipu S 1 1 Indian Institute of Tropical Meteorology, India, 2 Pukyong National University, korea In this paper we discuss the extent of Black Carbon (BC) radiative forcing in total aerosol atmospheric radiative forcing over Pune, an urban site in India. Collocated measurementsof aerosol optical properties, chemical composition and BC were carried out for a period of six months (during October 2004 to May 2005) over the site. Chemical composition data sets of water soluble, insoluble and BC components were used in Optical Properties of Aerosols and Clouds (OPAC) to derive aerosol optical properties for composite aerosols. The BC fraction alone was used in OPAC to derive optical properties solely for BC aerosols. The aerosol optical properties for composite aerosols and BC aerosols were separately used in SBDART model to derive aerosol radiative forcing due to composite aerosols and solely due to BC aerosols. The atmospheric radiative forcing for composite aerosols were found to be +35.5, +32.9 and +47.6 Wm -2 during post-monsoon, winter and pre-monsoon seasons respectively. The average BC mass fraction found to be 4.83, 6.33 and 4 µgm -3 during the above seasons contributing around 2.5 to 6% to the total aerosol load. The atmospheric radiative forcing estimated due to BC aerosols was +18.8, + 23.4 and +17.2 Wm -2 , respectively during the above seasons. The study suggests that even though BC contributes only 2.2 to 6% to the total aerosols load; it is contributing an average of around 55% to the total lower atmospheric aerosol forcing due to strong radiative absorption, and thus enhancing greenhouse warming.
STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 Formation of Interstellar Bubbles due to Asymptotic Giant Branch Wind: Eight New Bubbles Purposed Panthi Rajesh Tribhuvan University I present the results of numerical simulations for the first 10 4 years of the development of spherically symmetric interstellar bubble formed by the Asymptotic Giant Branch (AGB) wind. Assuming three phase interstellar medium (ISM) model we estimate the size of the interstellar bubbles. Our result will be based on 10 6 virtual stellar wind particles and discussed in the context of early and late AGB star. In addition to the numerical simulations, we systematically searched the bubble like structure in the 60 μm and 100 μm IRASS (Infrared Astronomical Satellite Survey) and measured their sizes. A comparison between the results of the numerical simulations and the observations is discussed. It is found that the size of the interstellar bubble lie in the range 1.48 pc to 39.20 pc if the stellar wind speed is 15 km s - 1 (early AGB wind). The size of the bubble ranges 2.82 pc to 74.64 pc if the stellar wind speed goes to 75 km s -1 (i.e., late AGB phase). The cold ISM forms small-sized bubble whereas the hot ISM produces large-sized bubble. However the stability of cold interstellar bubble is higher than that of the hot interstellar medium. As a preliminarily investigation we propose 8 interstellar bubble candidates, probably shaped by the White Dwarf and the Pulsar. The first four candidates are relatively small-sized (major diameter < 0.88 pc) because of the low speed stellar wind emitted during the evolution of White Dwarfs. The last four bubble candidates are intermediate sized, probably shaped by the relativistic wind of the Pulsar. The emission feature of the outer shocked region should be studied in the future in order to justify the nature of the interstellar bubble.
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scostep 2010 (stp12) - Leibniz-Institut für Atmosphärenphysik an der ...

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