Chemically Peculiar Stars Dennis Lamenti A540, Prof. Pilachowski Spring 2007.

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Presentation transcript:

Chemically Peculiar Stars Dennis Lamenti A540, Prof. Pilachowski Spring 2007

Outline History Identifying CP Stars Classification –Description of types Overall Properties Explanation of Peculiar Abundances Evolution of CP Stars

History 1897 Antonia Maury 1931 W.W. Morgan Eu II, Cr II varied in HD Horace Babcock, dipolar B field 78 Virginis 1958 Babcock, Catalogue of similar dipolar stars 1974 Preston classification

How are CP stars identified? Peculiar and/or variable line strengths Quadrature of line variability with radial velocity changes Photometric variability with same periodicity Slow rotation inferred by sharp spectral lines Some with rapid oscillations Variable strength of magnetic fields

T eff < 7000K homogenous 7000 < T eff < 30,000K

CP Classification Classical Name Preston Group Discovery criteriaSpectral Types Temp (K) Range Boo Weak Mg II, weak metalsA0-F Am-FmCP1Weak Ca II, Sc II, enhanced metals A0-F ,000 Bp-ApCP2Enhanced Sr, Cr, Eu, SiB6-F ,000 HgMnCP3Enhanced Hg II, Mn IIB6-A010,500-16,000 He-weakCP4Weak He IB2-B814,000-20,000 He-richEnhanced He IB220,000-25,000 Smith, K.C., 1996

Boo First spectrum 1943 MK&K Characteristics in visual (Gray 1988,1991): Weak Mg II 4481 Ca II K-line type of A0 Hydrogen-line type btwn A0-F0 Weak metallic-line spectrum ~50 Boö stars known (Gray & Corbally 2002) No detectable magnetic field (Shorlin, et.al 2002) IUE noted strong C I

Am-Fm Metallic lines classified by Titus & Morgan (1940) MK classification Roman, Morgan & Eggen (1948) Characteristics in visual: Weak Ca II K-line Strong metallic lines Slow rotation High Binary frequency No magnetic field detected (Shorlin, et.al 2002) Best known Am star is Sirius

Bp-Ap Several spectroscopic types (Jaschek & Jaschek 1958) SiCrEu, SrCrEu, Si, Sr Strong Magnetic Field (Shorlin, et.al 2002) Slow rotation Subset roAp (rapidly oscillating) Few mins period Small amplititude (~mmag) oscillation

HgMn 1906 Lockyer & Baxendall unable to id lines at 3944, 3984,4137,4206 & 4282 Å 1931 Morgan id 13 stars with spectra similar to prototype  And, thus put these into a classification 1914 Baxendall all but 3984 were Mn lines 1961 Bidelman showed 3984 Å as Hg II Slow rotation No detecable magnetic fields (Shorlin, et.al 2002)

He-weak 1960 Bidelman spectrum of 3 Cen A B5 star with weak He I Sharp lines P II, Ga II and noble gas elements 1961 Jugaku & Sargent  Scl B4 star weak He I Cr II, Ti II and Sr II Subclasses P-Ga (Phosphorus stars) 3 Cen A Sr-Ti  Scl stars Si (blue helium-weak stars, Jaschek & Jaschek, 1974) Slow rotation Magnetic Field (Shorlin, et.al 2002)

He-rich Consider only intermediate helium stars 1958  Ori E (Greenstein & Wallerstein) Classified from other He rich stars by normal H lines and Population I space velocities Magnetic fields (Shorlin, et.al 2002)

Location on HR diagram Open cluster data (North, 1993)

Frequency of CP Frequency by spectral type from BSC Smith, K.C., 1996

Rotational Velocity Smith, K.C., 1996

Frequency in Binary Systems Smith, K.C., 1996

Element Abundances Smith, K.C., 1996

Dipolar B Field Kochukhov et al. 2004

Explanation of Peculiar Abundances? Radiation Diffusion –Michaud 1970 Selective Accretion –Havnes, Conti 1971

Radiative Diffusion Theory Michaud, 1986

Selective Accretion Havnes, Conti 1971

Evolution of CP Stars Gomez, 1998

Evolution of CP Stars Hubrig, 2000

Evolution of CP Stars Pöhnl, et.al., 2003

Current Work Origin of Magnetic Fields –Fossil or dynamo Evolution of CP2 –Peculiar at ZAMS –Peculiar after 30% of MS lifetime –Parallel evolution of spectroscopic and magnetic peculiarities Diffusion model does not work for some element abundances Atmospheric modeling to include magnetic fields Non-LTE models

References Babcock, H 1947 PASP…59…260b Gomez, et.al A&A 336: Hubrig, et. al Ap.J. 539:352 Institute for Astronomy, University of Vienna, “The Delta a and Stellar Aggregates Research Group”, 12/03/07 Kochukhov, et.al A&A 424:935 Pöhnl, et.al A&A 402: Preston, George 1974 Annu. Rev. Astro. Astrophys. 12: Shorlin, et.al A&A 392: Smith,K.C Ap&SS 237: Image Credit M3, N.A.Sharp, Vanessa Harvey/REU program/NOAO/AURA/NSF