Context : Because of their relatively simple morphology , “ bubble ” H II regions have been instrumental to our understanding of star formation triggered by H II regions .
With the far-infrared ( FIR ) spectral coverage of the Herschel satellite , we can access the wavelengths where these regions emit the majority of their energy through their dust emission .

Aims : We wish to learn about the dust temperature distribution in and surrounding bubble H II regions and to calculate the mass and column density of regions of interest , in order to better understand ongoing star formation .
Additionally , we wish to determine whether and how the spectral index of the dust opacity , \beta , varies with dust temperature .
Any such relationship would imply that dust properties vary with environment .

Methods : Using aperture photometry and fits to the spectral energy distribution ( SED ) , we determine the average temperature , \beta -value , and mass for regions of interest within eight bubble H II regions .
Additionally , we compute maps of the dust temperature and column density .

Results : At Herschel wavelengths ( 70 \mu { m } to 500 \mu { m } ) , the emission associated with H II regions is dominated by the cool dust in their photodissociation regions ( PDRs ) .
We find average dust temperatures of 26 K along the PDRs , with little variation between the H II regions in the sample , while local filaments and infrared dark clouds average 19 K and 15 K respectively .
Higher temperatures lead to higher values of the Jeans mass , which may affect future star formation .
The mass of the material in the PDR , collected through the expansion of the H II region , is between \sim 300 M _ { \odot } and \sim 10 , 000 M _ { \odot } for the H II regions studied here .
These masses are in rough agreement with the expected masses swept up during the expansion of the H II regions .
Approximately 20 % of the total FIR emission is from the direction of the bubble central regions .
This suggests that we are detecting emission from the “ near-side ” and “ far-side ” PDRs along the line of sight and that bubbles are three-dimensional structures .
We find only weak support for a relationship between dust temperature and \beta , of a form similar to that caused by noise and calibration uncertainties alone .

Conclusions :