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GRB 041006 was detected by HETE-2 at 12:18:08 UT on 06 October 2004. This GRBdisplays a soft X-ray emission, a precursor before the onset of the main event,and also a soft X-ray tail after the end of the main peak. The light curves infour different energy bands display different features; At higher energy bandsseveral peaks are seen in the light curve, while at lower energy bands a singlebroader bump dominates. It is expected that these different features are theresult of a mixture of several components each of which has differentenergetics and variability. To reveal the nature of each component, we analysedthe time resolved spectra and they are successfully resolved into severalcomponents. We also found that these components can be classified into twodistinct classes; One is a component which has an exponential decay of $E_{p}$with a characteristic timescale shorter than $\sim$ 30 sec, and its spectrum iswell represented by a broken power law function, which is frequently observedin many prompt GRB emissions, so it should have an internal-shock origin.Another is a component whose $E_{p}$ is almost unchanged with characteristictimescale longer than $\sim$ 60 sec, and shows a very soft emission and slowervariability. The spectrum of the soft component is characterized by either abroken power law or a black body spectrum. This component might originate froma relatively wider and lower velocity jet or a photosphere of the fireball. Byassuming that the soft component is a thermal emission, the radiation radius isinitially $4.4 \times 10^{6}$ km, which is a typical radius of a bluesupergiant, and its expansion velocity is $2.4 \times 10^{5}$ km/s in thesource frame.

Multiple Component Analysis of Time Resolved Spectra of GRB041006: A Clue to the Nature of Underlying Soft Component of GRBs