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X-rays and planet formation. X-rays from young stars Magnetic reconnection flaring Some results from COUP & XEST Do X-ray flares influence planet formation? Evidence for X-ray irradiation of disks Implications of flare irradiation. Eric Feigelson (Penn State).

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X-rays and planet formation

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    1. X-rays andplanet formation • X-rays from young starsMagnetic reconnection flaring • Some results from COUP & XEST • Do X-ray flares influence planet formation? • Evidence for X-ray irradiation of disks • Implications of flare irradiation Eric Feigelson (Penn State) From Stars to Planets Apr 2007

    2. X-rays and star/planet formation Orion Nebula cluster & proplyd Star formation occurs in molecular cloud cores at T~10-100 K. Planet formation occurs in disks at T ~100-1000 K. This is neutral material (meV).

    3. But high energy radiation is present in planet formation environments: keV photons & MeV particles are produced in violent magnetic reconnection flares. Does this influence disk processes? (heating, ionization, chemistry, turbulence, viscosity, shocks, melting & spallation of solids) Theory looks good Is there evidence for X-ray/flare effects in disks, extrasolar planets & meteorites? Fe 6.4 keV & NeII 12.81mm, meteorites

    4. Some useful references • X-rays from young stars & stellar clusters Protostars & Planets V review article 2007 Feigelson, Townsley, Guedel & Stassun • ~20 papers from COUP ApJ Suppl Special Issue October 2005 + others 2006-07 • ~15 papers from XEST Special Issue As&Ap 2007 • ~5 papers/month on X-rays SFRs & disks

    5. The Chandra Orion Ultradeep Project 13-day observation of the Orion Nebula 1616 COUP sources: 849 low-NH ONC stars 559 high-NH stars, incl. 75 new members 16foreground stars 159 probable AGN 23 uncertain Getman & 22 others 2005 COUP #1 & #2

    6. COUP: The Movie

    7. Extraordinary flares inOrion pre-main sequence stars 1 2 JW 738 K=10.5 Age ~ 10 Myr Mass ~ 1 Mo log Lp = 32.6 erg/s X-ray cts / ks Time (13.2 days) Wolk et al. 2005 COUP #5

    8. X-ray luminosity fn spans 28 < logLx < 32 erg/s Correlation with stellar mass plus scatter There is no X-ray quiet population for M<3 Mo All X-ray sources are dominated by flares Guedel et al. XEST #1

    9. Characteristics of PMS flaring • Orion flares are typically 102 stronger than >X9 solar • flares releasing 1035-1036 ergs (0.5-8 keV). Many • smaller flares (powerlaw distribution like Sun/stars). • Flares occur every few days and last ~2-20 hrs • Flares unrelated to accretion variations and are • independent of presence of disks • Flare lightcurve & spectral evolution are usually • similar to solar/stellar flares • X-ray energies often extend to >10 keV

    10. Pre-main sequence X-rays are generally not produced by the accretion process ~15-day light curve X-ray flares Optical accretion event No relation seen between X-ray flares and accretion variations in ~800 Orion stars. Stassun et al. 2006/7 COUP #15/16 No difference in X-ray flaring of ~100 Class II vs. Class III Taurus stars. Stelzer et al. XEST #11

    11. Solar/stellar X-rays arise from magnetic reconnection events in the corona X-ray Sun -- Yohkoh Yokohama & Shibata 1998

    12. T Tauri X-rays arise from a complex reconnecting magnetosphere Both smaller (<1 R*) and giant (~10 R*) loops are inferred from COUP Flaccomio et al. 2005 Favata et al. 2005 COUP #6 & 7 Open accreting field lines Closed plasma-filled field lines Resulting X-ray corona (without flares) Jardine et al. 2006

    13. X-ray emission elevated throughout planet formation epoch 1 Mo X-ray levels are roughly constant during Class I-II-III phases … but drop greatly on the main sequence 0.5 Mo 0.2 Mo Preibisch & Feigelson 2005 COUP #4

    14. Three lines of evidence that X-rays irradiate protoplanetary disks • Some systems show evidence of X-ray reflection off of the disk: the fluorescent 6.4 keV iron line Imanishi et al. 2001, Tsujimoto et al. 2005, Favata et al. 2005 • Some systems show soft X-ray absorption attributable to gas in the disks Kastner et al. 2005 • Some systems show [NeII] IR line Glassgold et al. 2006, Pascucci et al. 2007

    15. Iron fluorescent lineCold disk reflects flare X-rays COUP spectra YLW 16A: protostar in Oph Imanishi et al. 2001 Tsujimoto & 7 others 2005 COUP #8

    16. X-ray absorption by gas in edge-on Orion proplyds First measurement of gas content of UV-irradiated photoevaporating disks? Kastner & 7 others 2005 COUP #9

    17. X-ray influence on planet formation Mag field lines Cosmic rays Flare X-rays Proto-Jupiter Proto-Earth Flare MeV particles Dead zone Ionized MHD turbulent zone Feigelson 2003, 2005

    18. X-rays & disk ionization YSO X-ray ionization rate dominates CRs in the disk by 108 for 1Mo PMS star at 1 AU: z = 6x10-9 (Lx/2x1030 erg s-1) (r/1 AU)-2 s-1 The ionization fraction is uncertain due to recombination processes. Hard (5-15 keV) X-rays should penetrate 1-100 g/cm2. Igea & Glassgold 1997 & 1999; Fromang et al. 2002; Matsumura & Pudritz 2003 & 2006; Alexander et al. 2004; Salmeron & Wardle 2005; Ilgner & Nelson 2006; Glassgold et al. 2007; Nomura et al. 2007 Reviews: Glassgold et al. 2000 PPIV & 2006; Balbus ARAA 2003; Dutrey et al. PPV 2007; Bergin et al. PPV 2007

    19. Plausible X-ray/flare effects on protoplanetary disks • PMS X-ray ionization will heat gas and change chemistry in disk outer layers. • PMS X-rays may be an important ionization source at the base of bipolar outflows. • X-ray ionization is likely to induce MRI turbulence affecting accretion, planetesimal formation, migration, ... • Flares may help explain enigmas in the meteoritic record: short-lived radionuclides, chondrule flash melting

    20. X-ray ionization of the gaseous disk PREDICTION Atomic excitation calculation of J1/2 J3/2 [NeII] 12.81 mm line from ionized outer layer of disks around 5-10AU Glassgold et al. 2006 DETECTION Spitzer FEPS Legacy reports [Ne II] line in 4 older, X-ray bright T Tauri stars Pascucci et al. 2007

    21. Protoplanet migration in a turbulent disk X-rays  MRI  MHD turbulence  inhomogeneities producing gravitational torques which overwhelm the Goldreich-Tremaine torque, so protoplanets undergo random walks rather than secular Type I migration. Gap formation suppressed. Laughlin et al. 2004 and other groups

    22. Conclusions • The X-ray studies of young stars show that powerful magnetic flares are ubiquitous throughout the epoch of planet formation. The astrophysics resembles solar flares • X-rays can efficiently irradiate protoplanetary disks Evidence: Fe fluor lines Absorption Possible consequences: Ionization Turbulence Heating Chemistry Chondrule melting Outflows CAI isotopes Therefore …..

    23. Planetary systems form in cool dark disks …. which are irradiated by 10 8violent magnetic reconnection flares