[mesa-users] L/L_edd>1?

[Tomer Shacham]

Hi Matteo,
I disabled convection by setting the mixing length to zero above a certain
radius.
I'm actually working on a certain generalisation of Joss '73, so I know
what you're talking about,
 it's just not it... In my specific conditions there is no inversion as you
can see in the attached graph,
(in which P and Rho were normalized to be in the same plot as L/Ledd)
Tomer


--
Tomer Shacham


High Energy Physics Group
Institute     of     Physics
The  Hebrew  University
Jerusalem,   Israel  91904



On 4 May 2014 20:54, Matteo Cantiello <matteo at kitp.ucsb.edu> wrote:

> Hi Tomer,
>
> On May 4, 2014, at 10:43 AM, Tomer Shacham <tomershacham at gmail.com> wrote:
>
> Hi Matteo,
> Since I disabled convection in the region I am referring to,
>
>
> Ok, then I'm not sure what's happening in your specific case (What do you
> mean you disabled convection?).
> I guess you'll have to produce some plots / share your inlist if you want
> more help at this point.
>
> But going back to your original question,  Lrad>Ledd is possible in
> stellar interiors in H.E (refs I shared with you in previous emails).
>
> Cheers,
>
> -M
>
>
> and I'm getting no gas pressure inversion,
> there must be some other reason.
> Best,
> Tomer
>
> --
> Tomer Shacham
>
>
> Astrophysics Group
> Institute     of     Physics
> The  Hebrew  University
> Jerusalem,   Israel  91904
>
>
>
> On 4 May 2014 20:33, Matteo Cantiello <matteo at kitp.ucsb.edu> wrote:
>
>> Hi Tomer,
>> the radiative luminosity can exceed the Eddington luminosity in H.E.
>> In that case the 1D solution to the stellar structure requires a gas
>> pressure inversion.
>> You are correct that convection sets in when the total luminosity exceeds
>> Ledd. See Fig. 39 in Paxton et al. 2013 and the analytics of Joss et al.
>> 1973
>> Cheers,
>>
>> -M
>>
>> On May 4, 2014, at 10:26 AM, Tomer Shacham <tomershacham at gmail.com>
>> wrote:
>>
>> Hi Matteo,
>> Thanks for your reply.
>> The Radiative luminosity cannot exceed Eddington, at least in the
>> hydrostatic limit. (Inside a star the total luminosity can exceed Eddington
>> only via convection.)
>> Best,
>> Tomer
>>
>> --
>> Tomer Shacham
>>
>>
>> High Energy Physics Group
>> Institute     of     Physics
>> The  Hebrew  University
>> Jerusalem,   Israel  91904
>>
>>
>>
>> On 4 May 2014 19:35, Matteo Cantiello <matteo at kitp.ucsb.edu> wrote:
>>
>>> Hi Tomer,
>>> I suggest you have a look at Sec. 7 of the second instrument paper
>>> (Paxton et al. 2013)
>>> where this issue is discussed at length.
>>>
>>> Overall, while at the stellar surface the stellar luminosity is limited
>>> by the Eddington Luminosity,
>>> deeper in the star it can (and it does in massive stars) exceed that
>>> limit.
>>>
>>> If in such cases the solution provided by 1D codes using MLT is a good
>>> approximation, well that's another story.
>>>
>>> -M
>>>
>>>
>>> On May 4, 2014, at 6:56 AM, Tomer Shacham <tomershacham at gmail.com>
>>> wrote:
>>>
>>> Dear Mesa-users
>>>
>>> Does anyone have an explanation for how is it possible for the radiative
>>> luminosity L_rad to be larger than the Eddington luminosity L_edd?
>>>
>>> (this happens almost always for high mass stars without using MLT++)
>>>
>>> Thanks,
>>> Tomer
>>> --
>>> Tomer Shacham
>>>
>>>
>>> Astrophysics Group
>>> Institute     of     Physics
>>> The  Hebrew  University
>>> Jerusalem,   Israel  91904
>>>
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