I think we need more time for coffee - doesn't all the actual work get done over coffee?
Anyway, it is Giant Planet Formation time...
Nope, we still don't understand it, in detail
like wtf is the deal with HR 8799?
And, yes, the sessions have been reshuffled,
this is to co-ordinate with the super secret mystery announcement from Kepler on thursday afternoon...
read about it here, or some boring NASA press release...
Liveblogging:
- Bromley on formation models, for giants natch
we're getting there, just not quite there yet...
can make loads of planets, in theory, just not always quite the right planets in quite the right places, at least we're at the stage where details matter.Disk lifetime is a key parameter for planet mass...
Hm, no more minimum mass solar nebula for us! - Morbidelli - Great Jumping Jupiters!
Covering the recent migrating Jupiter model - I am sooo jealous, had wanted a student to work on something similar
ah well, lots more fish in the ocean of ideaswe're getting frighteningly close to understanding the Solar System,
the revised Nice model does provide an interesting scenario, though I am a bit worried about bringing Jupiter all the way into 1.5 AU - Brad Hansen - in situ accretion of hot Neptunes and super Earths
- how to make intermediate mass planets in situ rather than migrate them in from the outer disk, like all sensible theorists like to do...definitely a tend away from minimum mass disk scenarios, it does help to have a lot of mass if you want to make funky systems
oligarchs or democrats, that is the question...
- Ruth Murray-Clay - core accretion at wide separation
some things to think about - Jane Greaves - imaging HL Tau B
oh noes, an observational interloper in the theory session!proto-planet imaging.
around class I low mass protostar with massive envelope
less than 100,000 years old
VLA imaging at 1.3 cm - sensitive to large dust grains
found, nice, at wide separation
looking for more using eMERLIN at 5cm - PEBBLES survey - Aaron Boley - disk instability formation
disk instability in outer parts of massive disks at early times, before inner disk settles to core accretion phase - links nicely to dust at 50-100 AU
clumps form - do they shear out or become bound
if bound what do they become?obligatory chuckle over "and magnetic fields..." (no they are not included, yet)
so, make clump, do chemistry in density enhancement, strip depleted gas tidally but that leaves the enriched dusty dense inner clump - that might do something interesting
Editorial comment: where is this large dust coming from - constant theme in this part of the session to have cm scale dust at large radii, but that just moves the question - where did this come from out there?
- Krattner - star formation -> planet formation
irradiation of star forming clumps
ok, we're done:
evening session is "Do we understand planet formation"
answer: No.
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You're making me regret my decision to not just crash this conference.
Hi Steinn -- thanks for doing this ESS blogging! Every morning this week I am checking to see the new developments from the previous day and I'm excited for the big Kepler announcement you mentioned.
With regards to Morby's talk, note that it is completely separate from the Nice model -- we call it the "Grand Tack" to represent the change in direction of Jupiter's migration (and because Kevin and Morby like to sail). So far it seems to work pretty well to explain the inner Solar System (and it has some pretty cool implications for the outer Solar System -- that's what I'm working on now). But we're always looking for concrete tests so if you come up with a good reason that Jupiter couldn't have migrated in to 1.5 AU let me know. So far the comment I get the most is that chondrules couldn't form beyond Jupiter's orbit (since in our model C-type asteroids originated past Jup) -- but my understanding is that the uncertainty in chondrule-formation models is awfully big....
cheers!
Sean
@tc - sadly we turned the conference over to aas conference management, and they are managing, so no sneaking in without a badge. Just got too big to run with an amateur SOC and no LOC.
@Sean - Hey Sean, you're another one who shoulda been here!
So, I actually like moving Jupiter, may still get a student (the student) to try a variation on that theme - from a theory perspective, coming all the way in to 1.5 AU and then back out again looks hard, requires a lot of gas to work with.
Agree the details of the meteorite/asteroid belt radial structure is a key, and your model looks to do that well, devil will be in the huge amount of detail data.
Probably won't be able to liveblog today's half-session, we're about to start and I have some paperwork to do which will preclude speed typing...
Hi again Steinn. I think we made a pretty good case that Jupiter and Saturn can migrate in and out in an evolving Solar Nebula (see http://adsabs.harvard.edu/abs/2011arXiv1107.5656P). What's still missing is a better treatment of gas accretion onto J/S during the migration. This is *key* since you need both the right masses and the right mass ratio for the Masset/SNellgrove mechanism to work. But not easy to do right! (We didn't in that paper but we're looking into it).
Look forward to the thursday blogging. Great stuff -- really helpful for those who couldn't make it there. I would love to have come but I have a new little guy (3 months old) and this is the older one's first week in school. Busy times!
cheers!
Sean
d'oh. oh well. Thanks for liveblogging the conference, though.
According to the pre-announcement announcement they've got someone from Industrial Light and Magic involved. So I'm guessing it is something about a circumbinary planet (Tatooine-like).
Why do people still like Star Wars these days anyway, it isn't particularly great and it is nearly 35 years old...
Hey Sean - don't worry... you've not missed too much theory-wise (though I liked the Lithwick / Wu secular chaos route for hot Jupiters, if you allow a bit of gas disk excitation of eccentricity). But tons of new observations, and Morby debating with Paul Kalas whether the Grand Tack is really a tack, in sailing terms, was a highlight... Phil
we're getting frighteningly close to understanding the Solar System,
the revised Nice model does provide an interesting scenario, though I am a bit worried about bringing Jupiter all the way into 1.5 AU
Does it explain why rocky planets form tens of millions of years after all the gas disappears? I was under the impression that meteroiticists were only getting more and more confused, as they acquire more data.
A youthful probably magenta Jupiter at 1.5 AU, what an awesome sight it must have been for anything that might have been alive on Earth then but wait...it is highly unlikely that the Earth got formed that early..oh well...
oh well, seem the world still didn't get the message of gemstone clouds in giant gas planets (and brown dwarfs) ... they are still wondering about haze formation although the ideas are out since 8 years. Maybe reading literature might help :-)
@Christiane - nowadays nobody reads papers that old - 5 years max - that way you can always claim to be first...