Can we determine the surface temperature of stars other than the Sun by using black body radiation theory? It is well known that the surface temperature of the Sun can be determined by fitting the solar spectrum with a black body radiation spectrum.
Is this scheme feasible for other stars?
Possibly the problem is obtaining the spectrum precisely.
 A: The question operates under a false premise. It isn't the case that fitting a blackbody spectrum to the Sun gives you its "surface temperature". On any detailed inspection, the Sun does not have a black body spectrum, although sometimes that approximation is made. A star cannot be characterised with a single "surface temperature".
What you can do is divide the luminosity of the Sun by $4\pi R^2 \sigma$, and this gives you $T_{\rm eff}^4$, where $T_{\rm eff}$ is known as the "effective temperature" and this is often what is being referred to when talking about the "surface temperature".
The effective temperature of a star is rarely deduced by dividing the luminosity by $4\pi R^2\sigma$, because for most stars we do not know their radius - this is actually the main difficulty in deducing an accurate $T_{\rm eff}$ for other stars. This is why the idea of fitting a blackbody function might be thought attractive. You can get an approximate answer in this way, but unfortunately, the photons in the real spectrum of a star come from different depths and at different temperatures depending on the wavelength considered and depending at what angle the line of sight makes to the stellar surface. The image below shows the real spectrum of the Sun compared with a blackbody at the $T_{\rm eff}$ implied by the Sun's luminosity and radius. Though you will sometimes see it said that this is the "best fitting blackbody spectrum", it isn't, although Wien's law would give you roughly the right answer.

In fact for most stars the $T_{\rm eff}$ is deduced by a detailed analysis of lots of spectral line features caused by the absorption due to various chemical elements in the atmosphere. For instance the ratio of line strengths due to iron atoms and singly ionised iron ions is a diagnostic of the temperature - at higher temperatures you get more ionisation. Similarly, higher temperatures lead to a greater population of excited states in an atom and this also leads to recognisable correlations between line strength and excitation energy that are diagnostic of temperature.
There are some types of star that are better fitted by a blackbody spectrum - very hot white dwarfs and perhaps hot neutron stars. But even there it is rarely the case that a blackbody spectrum is accurate enough to yield the correct temperature from a simple fit to the whole spectrum.
A: Yes of course. There are techniques which allow astronomers and astrophysicists to calculate these quantities quite efficiently and correctly and it depends on the spectrum, the luminosity and the distance of the star. In fact, from just the luminosity and the distance, one can compute almost everything important about the star including its age, composition, temperature, distance, mass and how much longer it will continue to live. A very useful book to study this at a relatively introductory level is the book by Prialnik (http://www.amazon.com/Introduction-Theory-Stellar-Structure-Evolution/dp/0521866049). A good advanced book is the book by Chandrasekhar (http://www.amazon.com/Introduction-Study-Stellar-Structure-Astronomy/dp/0486604136). 
However, I don't see where there is a spectrum problem because once you know the distance to the star and measure it's spectrum, you would need to account for the correct red-shift or blue shift and that's it. 
