How would the characteristics of a habitable planet change with stars of different spectral types? The tidal forces a habitable planet experiences increase with decreasing spectral type. So a habitable planet orbiting a smaller, less massive, and cooler star would experience much stronger tidal forces than one orbiting a bigger, more massive, and hotter star, and likely be tidally locked.
But what about other factors? How do other characteristics scale up with different stars?
For example would the orbital velocity of a planet in the habitable zone of a red dwarf be smaller than the velocity of a planet in the habitable zone of a more massive and hotter star?
The following table gives the mass, radius, temperature, and luminosity of an average star of several selected spectral types:
$$\begin{array} {d|c|c|} 
\text{Spectral Type} &amp; \text{Mass} (\odot) &amp; \text{Radius} (\odot) &amp; \text{Temperature (K)} &amp; \text{Luminosity} {(\odot)} \\ \hline
\text{M8V} &amp; \text{0.082} &amp; \text{0.111} &amp; \text {2500} &amp; {0.00043}\\
\hline
\text{M5V} &amp; \text{0.16} &amp; \text{0.199} &amp; \text {3030} &amp; {0.00299}\\
\hline
\text{M2V} &amp; \text{0.44} &amp; \text{0.434} &amp; \text {3550} &amp; {0.0268}\\
\hline
\text{K8V} &amp; \text{0.59} &amp; \text{0.587} &amp; \text {4000} &amp; {0.079}\\
\hline
\text{K5V} &amp; \text{0.68} &amp; \text{0.698} &amp; \text {4410} &amp; {0.165}\\
\hline
\text{K2V} &amp; \text{0.78} &amp; \text{0.763} &amp; \text {5040} &amp; {0.337}\\
\hline
\text{G8V} &amp; \text{0.94} &amp; \text{0.909} &amp; \text {5490} &amp; {0.673}\\
\hline
\text{G5V} &amp; \text{0.98} &amp; \text{0.982} &amp; \text {5660} &amp; {0.887}\\
\hline
\text{G2V} &amp; \text{1.02} &amp; \text{1.01} &amp; \text {5770} &amp; {1.014}\\
\hline
\text{F8V} &amp; \text{1.18} &amp; \text{1.25} &amp; \text {6170} &amp; {2.031}\\
\hline
\text{F5V} &amp; \text{1.33} &amp; \text{1.46} &amp; \text {6510} &amp; {3.434}\\
\hline
\text{F2V} &amp; \text{1.44} &amp; \text{1.61} &amp; \text {6810} &amp; {5.001}\\
\hline
\text{A8V} &amp; \text{1.67} &amp; \text{1.81} &amp; \text {7500} &amp; {9.3}\\
\hline
\text{A5V} &amp; \text{1.85} &amp; \text{1.94} &amp; \text {8080} &amp; {14.392}\\
\hline
\text{A2V} &amp; \text{2.05} &amp; \text{1.97} &amp; \text {8840} &amp; {21.263}\\
\hline
\end{array} $$
The following table gives the orbital distance, period, and velocity of an Earth-like planet receiving the same flux from its star as Earth does from the Sun, along with the radial velocity of the star caused by said planet and the tidal forces exerted on the planet relative to Earth:
$$\begin{array}{d|c|c|c|} 
\text{Spectral Type} &amp; \text{Orbital Distance (AU)} &amp; \text{Orbital Period (days)} &amp; \text{Orbital Velocity (km/s)} &amp; \text{Radial Velocity (m/s) } &amp; \text{Tidal Forces} {(\oplus)} \\ \hline
\text{M8V} &amp; 0.0207 &amp; 3.82 &amp; 59.166 &amp; 2.167 &amp; 9166\\ \hline
\text{M5V} &amp; 0.0547 &amp; 11.68 &amp; 50.929 &amp; 0.956 &amp; 977.34\\ \hline
\text{M2V} &amp; 0.163 &amp; 36.51 &amp; 48.812 &amp; 0.333 &amp; 100.09\\ \hline
\text{K8V} &amp; 0.281 &amp; 70.95 &amp; 43.134 &amp; 0.219 &amp; 26.5 \\ \hline
\text{K5V} &amp; 0.406 &amp; 114.84 &amp; 38.518 &amp; 0.17 &amp; 10.11\\ \hline
\text{K2V} &amp; 0.58 &amp; 182.93 &amp; 34.525 &amp; 0.133 &amp; 3.98\\ \hline
\text{G8V} &amp; 0.82 &amp; 280.06 &amp; 31.877 &amp; 0.101 &amp; 1.7\\ \hline
\text{G5V} &amp; 0.942 &amp; 337.48 &amp; 30.375 &amp; 0.093 &amp; 1.17\\ \hline
\text{G2V} &amp; 1 &amp; 365.56 &amp; 29.973 &amp; 0.088 &amp; 1\\ \hline
\text{F8V} &amp; 1.425 &amp; 572.18 &amp; 27.102 &amp; 0.068 &amp; 0.407\\ \hline
\text{F5V} &amp; 1.853 &amp; 799.11 &amp; 25.231 &amp; 0.057 &amp; 0.209\\ \hline
\text{F2V} &amp; 2.236 &amp; 1018.01 &amp; 23.901 &amp; 0.049 &amp; 0.128\\ \hline
\text {A8V} &amp; 3.049 &amp; 1505.21 &amp; 22.041 &amp; 0.039 &amp; 0.058\\ \hline
\text{A5V} &amp; 3.793 &amp; 1984.29 &amp; 20.799 &amp; 0.033 &amp; 0.033\\ \hline
\text{A2V} &amp; 4.611 &amp; 2526.01 &amp; 19.859 &amp; 0.029 &amp; 0.02\\ \hline
\end{array}$$

These calculations were done with the planet being at such a distance that it recieves exactly the same flux from its star as Earth does from the Sun. In reality a planet can be significantly farther away or closer and still remain in the habitable zone.
You can see a very clear correlation: As spectral type decreases (star becomes cooler, smaller, and less massive),

Orbital distance decreases,
Orbital period decreases,
Orbital velocity increases,
Radial velocity of the star increases,
Tidal forces on the planet increase exponentially.

I'm sure there are other factors that I didn't take into account but these are the most obvious ones I could think of.

1. I got the data for the mass, radius, and temperature of each star from here. This is an average relationship and not meant to be exact. 
2. The luminosity was calculated using the Stefan-Boltzmann law, assuming a perfect sphere and a blackbody radiator, which most stars approximately are.