Literature survey

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					Literature survey

    Shen Zhixia
    2004/03/18
Catalog
 Properties of SWPs: EUM04
 Planet system formation: GBWS04, Hal04,
  MLH04
 Pollution: BHSG04
 Disk evolution: IHMM04, JMMF04, Kle04,
  KLM04
 Detection: AS04
Properties of SWPs: EUM04
 Statistical properties of exoplanets
   III. Planet properties and stellar
 multiplicity
  –A. Eggenberger, S. Udry, and M. Mayor
  –Astro-ph/0402664
 Sample: 115 SWPs; 15 multiple star systems.
 Mass–period and the eccentricity–period
 diagrams
 Conclusion
  – The most massive short-period planets are all
    found in multiple star systems.
  – The planets orbiting in multiple star systems
    also tend to have a very low eccentricity when
    their period is shorter than about 40 days.
  – These observations seem to indicate that
    some kind of migration has been at work in
    the history of these systems.
Planet system formation:
GBWS04
 Early solar system radioactivity and AGB
  stars
 R. Gallino, M. Busso, G.J. Wasserburg, O.
  Straniero
 New Astronomy Reviews, 48:133
 This work studies the radioactive nuclei in
  the solar system to discuss the possible
  origin of our solar system.
 The possibility of a close-by AGB’s pollution
Planet system formation: Hal04
 Mixing, Volatile Loss and Compositional
  Change During Impact-driven Accretion of the
  Earth
 A. N. Halliday
 Nature, 2004, 427:505
 Modelling data from different radiogenic
  isotope system to discuss the mixing of new
  material and the losses of earlier accreted
  material in the growth of earth-like planets
Planet system formation: Hal04
 The model timescale for accretion from W is
  faster than current estimates based on terrestrial
  lead and Xe isotope data and Sr, W and lead
  data for lunar samples.
 Explanation: impacting core material did not
  always mix efficiently with the silicate portions of
  the Earth before being added to the Earth’s core.
 W & Sr : the Moon-forming impacting
  protoplanet was probably more like Mars, with a
  volatilerich, oxidized mantle.
Planet system formation: MLH04
 In-Situ Evidence for Live Iron-60 in the Early
  Solar System: A Potential Heat Source for
  Planetary Differentiation from a Nearby
  Supernova Explosion
 Mostefaoui, G. W. Lugmair and P. Hoppe
 Lunar and Planetary Science,2004,35:127
 The excess of 60Ni the existence of 60Fe in
  early age of the solar system.
 Origin from a nearby SN
 A possible heating source in planet system
Pollution: BHSG04
 ON THE CARBON AND NITROGEN
  ABUNDANCES OF 47 TUCANAE’S
  MAIN-SEQUENCE STARS
 Michael M. Briley, Daniel Harbeck,
  Graeme H. Smith and Eva K. Grebel
 AJ, 2004,127:1588
 Analysis of CN and CH band strengths of
  ~100 stars in 47 Tuc
Pollution: BHSG04
 Results:
Pollution: BSHG04
 Results:
   – A strongly anticorrelated relationship is seen between
     [C/Fe] and [N/Fe], with the CN-strong stars exhibiting
     depleted carbon and enhanced nitrogen.
   – The abundances of both elements agree remarkably
     well with those found among the evolved red giants of
     the cluster
   – In 47 Tuc the pattern of C depletions and N
     enhancements is quite similar to M71; while larger C
     depletions are evident in the more metal-poor cluster
     M5.
 Explain: pollution in early stage of the cluster
Disk evolution: IHMM04
 Transport Processes and Chemical Evolution
  in Steady Accretion Disk Flows
 M. Ilgner, Th. Henning, A. J. Markwick and T.
  J. Millar
 A&A, 2004, 415:643
 The model results:
  – Mass transport processes give influence globally
    on chemical evolution of the disk
  – Information about the local conditions is needed
Disk evolution: JMMF04
 DESTRUCTION OF STELLAR DISKS BY
  PHOTOEVAPORATION
 D. Johnstone, I. Matsuyama, I.G.
  McCarthy and A.S. Font
 Astro-ph/0402655
 Photoevaporation:
  – explain the short life of disk around a young star
  – Formation of a gap
  – Possible halting mechanism
Disk evolution: Kle04
 EVOLUTION OF PLANETS IN DISKS
 W. Kley
 astro-ph/0402642
 Review of the exo-planets:
   – Large Masses (0.2-17 MJup)
   – Small Distance (0.04 - 3.3 AU)
   – Large Eccentricities (0.0 - 0.91)
   – Resonant Orbits (2:1, 3:1)
   – Free Floaters (in Jupiter-mass range)
Disk evolution: Kle04
 Modeling embedded planets: assuming
 protoplanets have already been formed
Disk evolution: Kle04
 Modeling resonant planetary systems
Disk evolution: KLM04
 Discovery of a large dust disk around the
  nearby star AU Microscopium
 P. Kalas, M. C. Liu, B. C. Matthews
 Astro-ph/0403132
 AU Mic:
  – M star
  – 10 pc
  – Disk: 50-210 AU
Detection: AS04
 The detectabilitity of extrasolar planet surroundings: I.
  reflected light photometry of unresolved rings
 L. Arnold and J. Schneider
 Astro-ph/0403330
 Possibility:
   – the emitted thermal infrared light from the planet: no
     phase effect while the reflected visible light will vary
     versus the phase angle.
   – Photometric variation of the reflected light and the
     orbital phase of the ringsring:could be detected
Detection: As04

				
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posted:5/22/2013
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