How to convert magnitudes to bolometric luminosity? If we know a star's magnitudes from several bands(say u,g,r,i,z,J,H,k) and the star's distance, how to calculate Lbol?

Let's suppose the star has a black body spectrum. Is there any manual about the calculation? It's better to have a lot of technical details.
Quoting from Wikipedia,


  The bolometric magnitude Mbol, takes into account electromagnetic
  radiation at all wavelengths. It includes those unobserved due to
  instrumental pass-band, the Earth's atmospheric absorption, and
  extinction by interstellar dust. It is defined based on the luminosity
  of the stars. In the case of stars with few observations, it must be
  computed assuming an effective temperature. Classically, the
  difference in bolometric magnitude is related to the luminosity ratio
  according to:


$ M_{bol,*} - M_{bol,sun} = -2.5log_{10}(\frac{L_*}{L_{sun}})$


  In August 2015, the International Astronomical Union passed Resolution
  B2[7] defining the zero points of the absolute and apparent bolometric
  magnitude scales in SI units for power (watts) and irradiance (W/m2),
  respectively. Although bolometric magnitudes had been used by
  astronomers for many decades, there had been systematic differences in
  the absolute magnitude-luminosity scales presented in various
  astronomical references, and no international standardization. This
  led to systematic differences in bolometric corrections scales, which
  when combined with incorrect assumed absolute bolometric magnitudes
  for the Sun could lead to systematic errors in estimated stellar
  luminosities (and stellar properties calculated which rely on stellar
  luminosity, such as radii, ages, and so on).


[leading to the accepted definition of]
$ M_{bol} = -2.5log_{10}(L_*) + 71.1974... $ , where the constant term is the zero-point luminosity $L_0$ .

Dunno if this helps, other than that you have to determine the spectral luminosity of the star in question.