Jennifer Baerny

Publications (15) View all

• Source

  Available from: iccworkshops.org

  Article: Diagnostics for Lab and Astrophysical Plasmas

  J. K. Baerny, S. Woodruff, C. Smith
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  ABSTRACT: To monitor effects of vacuum conditioning, three radiation diagnostics are being built: a Helium–Neon (HeNe) heterodyne interferometer, a Bolometer, and a Hydrogen-alpha (Hα) detector. The interferometer will measure the line-average refractive index of the plasma, enabling us to obtain the line average density. The bolometer is a soft X-ray/UV detector (similar to those used on the Sustained Spheromak Physics Experiment (McLean et al. in Rev. Sci. Instruments 72(1):556–561, 2001) and the High-Beta Tokamak Experiment (Xiao and Navratil. in Rev. Sci. Instrument 67(9):3334–3335, 1996) and is used to directly measure the radiation loss from photons. The Hα detector will detect the amount of Hα being emitted by the plasma as a function of time, thus gauging the neutral density. These same concepts are also applied to astrophysical plasmas, with slightly different approaches. A brief overlap between diagnostics/detectors for laboratory and astrophysical plasmas is discussed. KeywordsInterferometry-Bolometry-Hydrogen-alpha detection-Astrophysical plasma diagnostics
  Journal of Fusion Energy 04/2012; 29(6):510-516. · 0.52 Impact Factor
• Source

  Available from: iccworkshops.org

  Article: Diagnostics for Lab and Astrophysical Plasmas

  J.K Baerny, S. Woodruff, C. Smith
  [show abstract] [hide abstract]
  ABSTRACT: To monitor effects of vacuum conditioning, three radiation diagnostics are being built: a Helium–Neon (HeNe) heterodyne interferometer, a Bolometer, and a Hydrogen-alpha (Hα) detector. The interferometer will measure the line-average refractive index of the plasma, enabling us to obtain the line average density. The bolometer is a soft X-ray/UV detector (similar to those used on the Sustained Spheromak Physics Experiment (McLean et al. in Rev. Sci. Instruments 72(1):556–561, 2001) and the High-Beta Tokamak Experiment (Xiao and Navratil. in Rev. Sci. Instrument 67(9):3334–3335, 1996) and is used to directly measure the radiation loss from photons. The Hα detector will detect the amount of Hα being emitted by the plasma as a function of time, thus gauging the neutral density. These same concepts are also applied to astrophysical plasmas, with slightly different approaches. A brief overlap between diagnostics/detectors for laboratory and astrophysical plasmas is discussed.
  Journal of Fusion Energy 01/2010; 29:510-516. · 0.52 Impact Factor
• Conference Proceeding: A Search for Galactic Halo and Thick Disk Planetary Nebulae in the SDSS Footprint: First Results

  Snedden, Stephanie, D. Oravetz, A. Simmons, J. Baerny, C. MacLeod, B. Balick, D. Bizyaev, H. Brewington, O. Malanushenko, V. Malanushenko, K. Pan, S. Watters, K. Anderson, J. Lutz, A. Kniazev, K. Kwitter, SDSS Collaboration
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  ABSTRACT: We present early results from a search for Galactic halo and thick disk planetary nebulae (PNe) within the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) imaging footprint. Known PNe of high and low excitation states cover a broad region in SDSS filter color-color diagrams. This space overlaps the areas where white dwarfs, quasars, A stars and emission line galaxies fall, and makes identification, from SDSS colors alone, difficult. We describe a search strategy that employs the SDSS colors, [O III] narrowband imaging and spectroscopy, and present the early results of the search for PN candidates with strong [O III] emission lines, from the first four months of observations.
  American Astronomical Society, AAS Meeting #211, Austin, TX; 01/2008
• Conference Proceeding: The Hubble Catalog of Planetary and protoPlanetary Nebulae

  Balick, Bruce, K. Pomeroy, S. Hayward, J. Baerny
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  ABSTRACT: We have downloaded, processed, and coadded every image of a planetary nebula (PN) and protoPN obtained with Hubble WFPC2 and ACS and available in the HST archives as of May 2006 (≈3700 images). Our immediate aim is to construct a high-resolution multi-filter catalogue of PNe and protoPNe to be posted on the web, along with image coordinates and primary references. The next step in our work is to look anew at the range of PN and pPN morphologies. We will define new morphological classes and sequences separately for PNe and protoPNe, examine the frequencies of defining characteristics in the sample, and relate the observed symmetries to various types of theories for AGB mass ejection and subsequent mass shaping processes such as fast stellar winds. Already it is clear that the shapes of protoPNe are more various and complex than those of most PNe, showing that the structures initially imposed by AGB mass ejections are blurred by the momenta of ionization fronts and fast stellar winds that come later. The final step will be to relate the morphologies of protoPNe to the evolutionary stages of their central stars. This research is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. Support for this work was provided by NASA through grant number AR-10933 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555.
  2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, Seattle, WA; 01/2007
• Conference Proceeding: The Selection of RR Lyrae Stars Using POSS and SDSS

  Fraser, Oliver J., J. R. Barton, B. J. Oldfield, T. P. Biesiadzinski, D. A. Horning, J. K. Baerny, F. Kiuchi, D. Krogsrud, D. S. Longhurst, L. P. McCommas, J. A. Scheidt, R. Covarrubias, K. Covey, C. Laws, B. Sesar, Z. Ivezic
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  ABSTRACT: We test a method for identifying candidate RR Lyrae stars based on a comparison of POSS and SDSS photometry (Sesar et. al. 2005). Our candidate stars range in SDSS g magnitude from 14.4--16, or a distance of 6--12 kpc. Follow-up photometry obtained at Manastash Ridge Observatory typically includes 30-40 points per light curve. We find that at least two thirds of our sample of 23 objects are clearly variable, with light curves consistent with RR Lyrae. Candidate RR Lyrae were selected using stars that had brightened at least 0.3 magnitudes between POSS and SDSS, and which had SDSS magnitudes and colors consistent with the cuts in Ivezic et al. 2004.
  2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, Seattle, WA; 01/2007