Definition of Super-Earth

Interesting. Also John M. Dollan typed a similar classification for his ArcBuilders' Universe but this one adds one more subtype

I have some questions to put you down:

What is the theoretical minimal
mass for a gaseous planet?

What is the intervalley of mass for a " neptunian " planet?
Is it 30MT the maximum? (HARPS had concentrated on on the study of superearths and of neprunians planets and the border was 30ME)

Tx

I think the minimum mass should be around 0.022 and upper limit 0.15 Jupiter masses. Ask Lazarus, he's got many informations

>0.15Mj = metalic hydrogen??

Yes, likely

Even >0.22 Mj.

Look HD 149026b 2/3rds of its mass has been found to be rocky. So does HAT-P-3b.

Tx

I have another question. I know that I ask too much question. Excuse
me.
From what mass a superearth can have a mantel of hot ice?

I don't know. Maybe 1/3rd or planetary mass. Actually I don't own such data

I badly expressed myself. What must be the minimal mass of the planet so that of the hot ice is possible form?

I don't know. Ask Lazarus

Is Lazarus a member?

Stalker wrote:

Is Lazarus a member?

Yes, you must be a member to put posts on this site. This is to complicate matters a bit for spammers.

I must say that I've been very busy in "real life" for the past two weeks, and I shall be so for the next two as well. As such, I don't have as much time as I would like to have available, especially for fixing the annoying grey text in the post input fields. I promise though, I will work on it when I can.

Lazarus owns many informations about astronomy and astrophysics.
Recently we were discussing here. You may check profile and send a private message if you need:

https://solar-flux.forumotion.com/general-questions-f11/carbon-jovians-t33.htm

Tx

Welcome

Here's a phase diagram of water, you can see the hot ice phases on it. However the p/T range spanned by that phase diagram is not adequate to cover the conditions in planetary interiors. See also this paper which discusses the structures of ocean planets.

The "hot ice" issue is a tricky one, as it is complicated when the planet has internal heat or contains hydrogen. For example, Neptune and Uranus are predicted to be fluid (molecular at the top of the atmosphere, ionic in the mantle) throughout their interiors, possibly with the water and ammonia transitioning to a fluid metallic state near the core (see this paper for details). Thus I am sceptical that the planet Gliese 436b is going to have a solid "hot ice" mantle, as it is a hotter planet than either Uranus or Neptune. Note that both Uranus and Neptune are too hot and dry to support liquid water in the interior: see this paper.

Tank's Lazarus

Is possible be that there is not lower border as the hot ice.

Callisto
has a nucleus of constricted ice and of rock. The similar for the
mantel of Ganymède. Titan has a mantel of ice constricted
without rocks.

Stalker wrote:

Tank's Lazarus

Is possible be that there is not lower border as the hot ice.

Callisto
has a nucleus of constricted ice and of rock. The similar for the
mantel of Ganymède. Titan has a mantel of ice constricted
without rocks.

Yes, but objects you mean lay beyond system's snowline. It's exotic high pressure ice which plays an interesing role in Hot Neptunes, because they seem to form beyond host star's snowline (>2 AUs) and then migrate inwards, in "torch" orbits.

What about an Icy analog?

marasama wrote:

What about an Icy analog?

Something like Uranus and Neptune, right?