Anatoly Miroshnichenko

Experience

Observations

• The 6-m telescope with a medium-resolution TV scanner and high-resolution spectrographs, Special Astrophysical Observatory, Russia (1989-present, observing time have been allocated over 30 times)
• The 3.0-m NASA Infrared Telescope Facility with a Ge-bolometer (2 nights awarded in February 2000) and with IR-camera MIRLIN (6 half-nights awarded in October 2001)
• The 2.7-m Harlan Smith telescope of the McDonald Observatory with a coude echelle spectrograph (30 nights awarded in 2005, 2006, 2008, 2009, 2012)
• The 2.1-m Otto Struve telescope of the McDonald Observatory with the Sandiford echelle-spectrograph (4 nights awarded in October 2001, 5 nights in September 2002, 4 nights in December 2004)
• The 2.1-m telescope of San Pedro Martir Observatory (Baja California, Mexico) with an echelle spectrograph (4 nights awarded in October 2005, 5 nights in December 2006, 14 nights in November 2007, 14 nights in October 2008, 9 nights in November 2009, 6 nights in October 2010, 6 nights in November 2011, 2 nights in January 2012, 7 nights in November 2012, 8 nights in October 2013, 11 nights in September, October, and December 2014)
• The 1.5-m Carlos Sanchez Telescope of the del Teide Observatory in Canary Islands (4 observing runs in 1999-2001).
• 1.0-m telescopes with a two-channel optical and near-infrared photometer-polarimeter, Assy and Tien-Shan Observatories, Kazakhstan (1984-2002, more than 80 observational runs, more than 2000 multicolor photometric and polarimetric observations).
• 1.0-m telescope at the Ritter Observatory (University of Toledo, Ohio, USA) with a high-resolution spectrograph (05/97-06/98, 05/99-06/05).
• 0.81-m telescope of the Three College Observatory (TCO, University of North Carolina at Greensboro, near Snow Camp, NC, USA) with a high-resolution echelle spectrograph Eshel from Shelyak Instruments (since October 2011).
• 0.8-m telescope of the del Teide Observatory in Canary Islands (10 nights in 2011) with a high-resolution long-slit spectrograph LHiresIII from Shelyak Instruments.
• 0.4-m - 0.6-m class telescopes with optical and infrared photometers and polarimeters, Byurakan Observatory, Armenia (1979-1983, 5 observing runs).

Data reduction

• Author of several data reduction FORTRAN codes for photometry and spectroscopy, including algorithms of spectral line separation and analysis.
• Experience in medium- and high-resolution spectroscopic data reduction in different packages.
• Data reduction with the IRAF package: IRAS high-resolution maps, aperture photometry, echelle spectroscopy.
• Over 1000 spectra obtained at the 0.81-m TCO telescope have been reduced (spectral resolving power R ~12000, October 2011 - May 2014).

Computers and model calculations

• Calculation of Balmer emission line profiles in gaseous envelopes of early-type stars using the Sobolev approximation (non-LTE case, includes population calculations for 20-level hydrogen atom, all radiative and collisional processes are taken into account) in spherical and axisymmetric geometries.
• Calculation of continuum spectral energy distributions for stars with circumstellar gaseous envelopes in spherical and axisymmetric geometries.
• Calculation of continuum spectral energy distributions with the recently released DUSTY code (Ivezic, Nenkova, Elitzur 1999, Internal report, Univ. of Kentucky) solving radiation transfer equation in spherically symmetric dusty envelopes.
• Calculation of theoretical spectra with the code Synspec (Hubeny, Lanz, Jeffery, 1995, Synspec -- A User's Guide, Version 36).

Teaching and Lectures

• In 1985-1987 I delivered astronomy courses to groups from secondary schools at the Saint-Petersburg Planetarium.
• In 1987-1993 six undergraduate students of the Saint-Petersburg University completed their Diploma Theses under my supervision.
• In 2000 an undergraduate student A. Gault of the University of Toledo worked with me during the summer REU program and complied a new catalog of classical Be stars brighter than V=7.5 mag.
• In 1991-2002 I have been giving different talks in a number of astronomical institutes and observatories in Italy, Spain, Belgium, France, Russia, and USA.
• In 1997-2005 (twice a year) I have been giving talks on different astronomical subjects at a local Astronomy Seminar at the University of Toledo.
• In 2001 I got my first real experience in teaching an astronomy course ASTR 4810 at the University of Toledo.
• In the Fall 2003 I taught a course Survey of Astronomy ASTR 1010 at the University of Toledo.
• Two undergraduate courses, Survey of Astronomy and Survey of Natural Sciences, were taught in the Fall 2004 (University of Toledo)
• General Physics (PHYS2080, Electricity and Magnetism, Light and Optics, and Modern Physics) were taught in Spring 2005 (University of Toledo)
• Survey of Astronomy (AST 209/235) - since Fall 2005 at the University of North Carolina at Greensboro (UNCG)
• Physics Labs (PHY 325L, 211L/291L, 212L/292L) - since Fall 2005 at UNCG
• Astrophysics (AST 330) - Fall 2006, Fall 2008, Fall 2011, Spring 2013 at UNCG
• Individual study (PHY 496, Geoff Nichols) - Fall 2008
• Individual study (PHY 496, John Doll) -Fall 2010
• Individual study (PHY 496, Larkin Folsom) - Spring 2014
• Two students at UNCG (Keith Thomas and Angie Kapely) worked with me during Summer 2006 on projects concerning B[e] stars
• Larkin Folsom worked on anaysis of spectra of the Be star Beta Canis Minoris in 2013 and 2014. A poster on the project results was presented at the international meeting Bright Emissaries in London, ON, Canada, in August 2014 and at the North Carolina Astronomers annual meeting in Jamestown, NC, in October 2014.

Last updated:  2014 September 23