Mass, Radius, Colour, Size, Type of a Star from the Hipparcos Catalog Using data from the Hipparcos Catalog download file, is there a way to determine the Visual or Apparent Magnitude from the data within?

Can I obtain the Mass, Radius, colour, temperature, type (dwarf, sun-like, hypergiant, etc) of the star from the catalog?  Which column relates to which item i'm looking for?  Any examples?
The apparent magnitude (in V ~ visual) is in column 42-46. Other magnitudes are BT magnitude (columns 218-223) and VT magnitude (columns 231-236). These are magnitudes recorded with different (colour) filters. 
The colour ($B-V$) can be found in columns 246-251, expressed in magnitudes. This is the difference between V (visual) magnitude and B (blue) magnitude also known as the colour index. Blue stars have a low colour index ($B-V&lt;0$) as the star will be brighter in the blue (B) passband (filter), and will therefore have a low B magnitude, while red stars will have a higher $B-V$ colour index.

Mass, Radius, and Temperature are not in the catalogue. Mass can only be directly determined for multiple star systems and requires a lot of observations per multiple star. Radius is determined from stellar models. And Temperature can be determined from the spectrum of the star. A crude indication can be gotten from the colour index of the star. (see for instance this webpage).

Finally the type can be found in the star's spectral type. The spectral type is in columns 436-447. These spectral types are not always easy to read but they consist of a spectral class (e.g. O, or F type stars) and the luminosity class (and some other information). The luminosity class gives the type of class in roman numerals. Below is the list from the wikipedia page on stellar classification.


0 or Ia+ (hypergiants or extremely luminous supergiants). Example:
Cygnus OB2#12 (B3-4Ia+)[12] 
Ia (luminous supergiants). Example: Eta
Canis Majoris (B5Ia)[13] 
Iab (intermediate luminous supergiants).
Example: Gamma Cygni (F8Iab)[14] 
Ib (less luminous supergiants).
Example: Zeta Persei (B1Ib)[15] 
II bright giants. Example: Beta
Leporis (G0II)[16] 
III normal giants. Example: Arcturus (K0III)[17]
IV subgiants. Example: Gamma Cassiopeiae (B0.5IVpe)[18] 
V main-sequence stars (dwarfs), Example: Achernar (B6Vep)[15] 
sd (prefix) subdwarfs. Example: HD 149382 (sdB5)[19] 
D (prefix) white
dwarfs.[nb 2] Example: van Maanen 2 (DZ8)[20]


The Sun's spectral type is G2V, which means that the spectral class is G2 and the luminosity class is V, which means that the Sun is a main-sequence star.

An example:

The following record is for the star Arcturus (α Boötis):

H|       69673|H|14 15 40.35|+19 11 14.2|-0.05|1|G|213.91811403|+19.18726997|*|  88.85|-1093.45|-1999.40|  0.92|  0.42|  0.74|  0.60|  0.52|-0.52| 0.16|-0.13|-0.07| 0.05|-0.01| 0.03|-0.12|-0.03|-0.31|  7| 2.01| 69673| 1.629|0.010| 0.286|0.009|*| 1.239|0.006|G|1.22|0.02|A|*| 0.1114|0.0020|0.015| 70|*| 0.09| 0.14|       |U|2| |14157+1911|H| 1| 2|C| |A|AB|198|  0.255|0.039| 3.33|0.31|S| | |124897|B+19 2777 |          |          |1.22|K2IIIp      |X 


The apparent visual is(V) magnitude $-0.05$. The colour index is $B-V = 1.239$, which means that it is probably a red K type star with temperature $T\approx 4000 \textrm{K}$ (from figure 2 on this webpage). The spectral type is K2IIIp, i.e. the spectral class is K2 and the luminosity class is III, a normal giant star.

An indication for the Radius can be found from the Hertzsprung-Russel Diagram in which radii are added (see Figure here). The luminosity of Arcturus can be calculated as follows:
$$ d = \frac{1}{\varpi}$$
where $d$ is in parsec and $\varpi$ is the parallax in arsceconds. The parallax is in columns 80-86 and is $\varpi = 88.85mas = 0.08885^{\prime\prime}$ for Arcturus. The distance is, therefore, $d=11.25\textrm{pc}$. You can then calculate the absolute magnitude ($M_V$):
$$ M_V = m_V -5(\log{d}-1)$$
where $m_V$ is the apparent visual (V) magnitude. The absolute magnitude of Arcturus is: $M_V=-0.05 - 5(\log{11.25}-1)=-0.31$.
The luminosity is then given by:
$$M-M_{\textrm{sun}} = -2.5\log{\left( \frac{L}{L_{\textrm{sun}}}\right)}$$
where the absolute magnitude of the Sun is $M_{\textrm{sun}} = 4.83$ and $L$ is the luminosity of Arcturus. This gives:
$$\log{\left( \frac{L}{L_{\textrm{sun}}}\right)} = 2.056 $$
$$L = 114  \textrm{L}_{\textrm{sun}}$$
From the Hertzsprung-Russel diagram we get a radius for Arcturus of about $R \approx 10  \textrm{R}_{\textrm{sun}}$.