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    4.

    Assuming the sun to have a spherical outer surface of radius rr, radiating like a black body at temperature t0C{t^0}C, the power received by a unit surface, (normal to the incident rays) at a distance R from the centre of the sun is Where σ\sigma is the stefan’s constant.

    A

    4πr2σt4R2\frac{{4\pi {r^2}\sigma {t^4}}}{{{R^2}}}

    B

    r2σ(t+273)44πR2\frac{{{r^2}\sigma {{\left( {t + 273} \right)}^4}}}{{4\pi {R^2}}}

    C

    16π2r2σt4R2\frac{{16{\pi ^2}{r^2}\sigma {t^4}}}{{{R^2}}}

    D

    r2σ(t+273)4R2\frac{{{r^2}\sigma {{\left( {t + 273} \right)}^4}}}{{{R^2}}}

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    5.

    Assuming the sun to have a spherical outer surface of radius rr, radiating like a black body at temperature t0C{t^0}C, the power received by a unit surface, (normal to the incident rays) at a distance R from the centre of the sun is Where σ\sigma is the stefan’s constant.

    A

    4πr2σt4R2\frac{{4\pi {r^2}\sigma {t^4}}}{{{R^2}}}

    B

    r2σ(t+273)44πR2\frac{{{r^2}\sigma {{\left( {t + 273} \right)}^4}}}{{4\pi {R^2}}}

    C

    16π2r2σt4R2\frac{{16{\pi ^2}{r^2}\sigma {t^4}}}{{{R^2}}}

    D

    r2σ(t+273)4R2\frac{{{r^2}\sigma {{\left( {t + 273} \right)}^4}}}{{{R^2}}}

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