inti didn’t form in the x wind (and neither did most cais)
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Inti didn’t form in the X wind (and neither did most CAIs). Steve Desch Arizona State University Harold Connolly, Jr. CUNY Kingsborough. Outline of Talk. Diving into Inti Inti didn’t form in an X-wind... ...but it ended up in a comet anyway, because. Inti Introduced. - PowerPoint PPT PresentationTRANSCRIPT
Inti didn’t form in the X wind(and neither did most CAIs)
Steve DeschArizona State University
Harold Connolly, Jr.CUNY Kingsborough
Outline of Talk
• Diving into Inti
• Inti didn’t form in an X-wind...
• ...but it ended up in a comet anyway, because...
Inti Introduced
Comet 81P/Wild 2Scattered into present orbit in 1974; was previously a member of the Kuiper Belt Scattered Disk
Probably formed at 10-30 AU
Stardust Sample Track 25 called ‘Inti’. It’s a CAI, formed (by condensation) at > 1700 K.
Zolensky et al (2006)
X-wind windicated? Shu et al. (1996, 2001)
rockvapor ~ 10-12 g cm-3
1. Gas (H2), small (< 100 um) solids rapidly funneled away from CAI-forming zone
gas(H+) ~ 10-16 g cm-3
3. CAIs grow by evaporation / recondensation here
2. Large (> 100 um) “proto-CAIs” enter Reconnection Ring
4. CAIs flung by X-wind into comets.
X-wind = eXtra-oXidizing Gas in reconnection ring ionized, funneled onto star.
Shu et al. (2001) estimate (from protostellar X-ray emission) T= 8 x 106 K, ne = 108 cm-3 (gas ~ 10-16 g cm-3) between flares, in reconnection ring.
CAIs grow in reconnection ring by re-condensation following flares, from rock vapor (rockvapor ~ 10-12 g cm-3)
Fedkin & Grossman (2006)
Intrinsic fO2 of CAI vapor > IW+1 (Kozul et al. 1988)
CAIs form in reconnection ring, where fO2 ~ 106 x solar, near IW
Inti Revealed
Inti itself is small, < 10 microns
Inti contains within its spinel grains of osbornite, (Ti,V)N (likely condensates).
Redox ReduxfO2 during CAI formation known to be < IW-6 from Ti4+/Ti3+ ratios in fassaite and rhönite (Beckett 1986,
Krot et al. 2000)
Osbornite in Inti shows it also formed in the gas of the solar nebula!
Osbornite-bearing CAI recently found in CH/CB Isheyevo, recognized as formed in the solar nebula (Meibom et al. 2007), demands C/O = 0.91-0.94 (IW-7) (Ebel 2006)
Solar nebula ebb and flow
r (AU) 5 10 15 20 25 30
‘Nice model’ (Tsiganis et al. 2005; Gomes et al. 2005): the outer planets formed much closer to Sun
Minimum mass solar nebula (Weidenschilling 1977), with (r) r^(-1.50), must be updated!
Desch (2007) shows (r) r^(-2.17) !
Outer Solar Nebula = Decretion DiskAll viscously evolving disks viscously spread outward.
Mass distribution can be matched by a spreading disk, with outward mass flow (Desch 2007).
Steady-state solution with outward mass flow also matches (Desch 2007.) If (r) r^(-p) and T(r) r^(-q), mass must flow outwards if p+q > 2 (Takeuchi & Lin 2002)
Gas, CAIs moved from a few AU to > 10 AU in < 10 Myr
Desch (2007, in revision)
Conclusions•X-wind predicts fO2 where CAIs formed > IW. But CAIs overall formed in solar gas, < IW-6 (rhönite / fassaite), and Inti in particular at IW-7 (osbornite).
•Inti too small to enter reconnection ring as a proto-CAI; probably too small even to be ejected by X-wind.
•Nice model for initial planet positions used by Desch (2007) to derive new “minimum mass solar nebula”. Derived density profile so steep, mass must have flowed outward, from a few AU to > 10 AU in < 10 Myr.
•Inti (like all CAIs) formed in the solar nebula; it was transported by disk dynamics to comet-forming zone.