Vertical Structure Model for Passive Irradiated Circumstellar Disks

C.P. Dullemond, G-J. van Zadelhoff and A. Natta

Pre-main-sequence stars are often still surrounded by the remnants of the accretion disk from which they were born. In the late stages, when the active accretion has stopped or drops below a certain value, the disk is energetically dominated by the irradiation of its surface by radiation from the central star. These dust+gas disks emit a strong infrared continuum ranging from the near infrared to the millimeter.

In our paper "Vertical structure models for T Tauri and Herbig Ae disks", we present models in which the vertical structure of the disk is computed with full frequency- and angle-dependent radiative transfer. We refer to this paper for the details.

Vertical temperature profile Vertical temperature profile
The vertical temperature and density profile of the T Tauri disk model at 1 AU from the central star.

Downloading the models

Here you can find the model data files corresponding to the two models worked out in the paper. The first model is a disk around a T Tauri star, the second a disk around a Herbig Ae star.

NOTE:



 The model data are freely available. But use of the data for scientific publications is only allowed when our paper is properly referenced. If you plan to use the data for any kind of scientific purpose, we would be very glad if you send us a short email, so that we can keep track of who is using our model, and who to update in case of modifications and/or bugfixes.

Download T Tauri model
Download Herbig Ae model

The computer code for computing these models is not yet publically available (will be in the future). But if you are interested in using this code, you are welcome to contact me.

Simplified benchmark test cases

Apart from extensive internal-consistency-checking, we have made a number of test comparisons with independent codes in order to test the correctness of our models. As was to be expected, it turned out to be a non-trivial task, and it took quite a lot of our time. We decided to make these test cases available to the community for several reasons. First of all, we would like others to verify our results, and inform us about their findings. Secondly, these independent results can then be added to our list of results, and hopefully we converge on a single unique answer to all test problems. Once these benchmarks are established, they can be used by others in the astrophysics community to test their codes.

-------> THE TEST PAGE <-------

dullemon@mpia.de