# The viscous decretion disk model of the classical Be star $\beta$ CMi revisited

## TL;DR

This paper revisits the viscous decretion disk model of the Be star β CMi, correcting a software bug, and demonstrates that a single power-law density profile can explain observations, confirming key model predictions.

## Contribution

The study updates the VDD model with a corrected radiative transfer code, showing that a single power-law density profile suffices to explain observations of β CMi.

## Key findings

- Corrected the radiative transfer code, improving model accuracy.
- Demonstrated a single power-law density profile fits all observations.
- Confirmed disk truncation at 35 stellar radii remains valid.

## Abstract

We revisit the viscous decretion disk (VDD) model of the classical Be star $\beta$ CMi as presented by \citet{klement} using an updated version of the radiative transfer code {\ttfamily HDUST}. A software bug was causing the mean intensities to be slightly underestimated in the equatorial region of the disk, with small but detectable effects on the disk temperature and emergent spectrum. The new model fixes an unexplained feature of the original model, which was able to reproduce the observations only when considering a dual density behavior: a steep density fall-off in the very inner parts of the disk followed by a shallower density profile. The new model is able to reproduce all the observables reasonably well using a single power-law for the density profile throughout the whole disk, as predicted by the VDD model. All the other original conclusions, most importantly the reported truncation of the disk at the distance of 35 stellar equatorial radii from the central star, remain unchanged.