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Black Holes Research

Black Holes Research. By: Jesse Corley. Background info on M51. AKA the Whirlpool Galaxy, Rosse’s Galaxy, and Lord Rosse’s “Question Mark”. A spiral interacting galaxy. The larger galaxy is known as NGC 5194 (M51A) and the smaller galaxy is known as NGC 5195 (M51B).

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Black Holes Research

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  1. Black Holes Research By: Jesse Corley

  2. Background info on M51 • AKA the Whirlpool Galaxy, Rosse’s Galaxy, and Lord Rosse’s “Question Mark”. • A spiral interacting galaxy. The larger galaxy is known as NGC 5194 (M51A) and the smaller galaxy is known as NGC 5195 (M51B). • Discovered on October 13th, 1773 by Charles Messier while observing a comet and described it as “very faint nebula, without stars”. • The companion galaxy, NGC 5195, was discovered on March 21st, 1781 by Pierre Méchian. • The spiral structure was discovered in the spring of 1985 by Lord Rosse.

  3. Technical Aspects • Co-ordinates(J2000): RA: 13h 29m 52.37s DEC: +47⁰ 11’ 40.8” • Located in the constellation Canes Venatici, beneath the Big Dipper. • Distance: (23.1 +/- 3.9) Mly • Apparent dimension: 11’ X 7’ = (73 915 X 47 037) ly • Apparent magnitude: 8.8 • About the threshold of what a naked human eye can observe. • Is a spiral galaxy, type Sc. Type Sc refers to spiral galaxies with dominant, multiple spiral arms and amorphous nuclei.

  4. How black holes are formed • A star of at least and estimated 25 solar masses will use up its fuel through the fusion of lighter elements into heavier elements until there is no more fuel. http://stardate.org/images/gallery/sun5.jpg

  5. How black holes are formed • It will then not have enough pressure to counter gravity and so collapses. • First it collapses to the point where electron degenerancy tries to counter gravity, becoming a white dwarf, but since the star is too massive, its core will compress further. • The core compresses until electrons and protons combine to create neutrons and neutrinos. The star then goes… Credit: NASA, ESA, H. Bond (STScI), and M. Barstow (University of Leicester)

  6. How black holes are formed • what’s left is a neutron star, which tries to counter gravity by neutron degenerancy pressure, becoming a neutron star. • Credit: J. Hester (ASU) et al., CXC, HST, NASA

  7. How black holes are formed • Since the star is still too massive, it will undergo total gravitational collapse until it becomes a black hole. • Drawing Credit: XMM-Newton, ESA, NASA

  8. How black holes are formed • A black hole, however, does not need to start out as a black hole. As long as an object acquires enough mass, it can form a black hole. One example would be a star, such as a neutron star, colliding with another star of sufficient mass.

  9. How to detect black holes-Gravitational Lensing • According to Einstein’s General Theory of Relativity, massive objects can bend light. The more massive an object is, the more light bends around it. The effect is to brighten the object and to create several images of the object. • Credit: Andrew Fruchter (STScI) et al., WFPC2, HST, NASA

  10. How to detect black holes-Accretion Disks and X-Ray Binaries • In a binary system involving a black hole, the black hole can strip material off of its companion star, this forms an accretion disk. • This disk is a partially ionized gas, otherwise known as plasma. Due to complicated energy interactions in the plasma, electromagnetic radiation is given off, which peaks in the X-ray range for stellar mass black holes. • Credit: CXC, NASA; Illustration Credit: M. Weiss (CXC)

  11. How to detect black holes-Accretion Disks and X-Ray Binaries • X-rays and radio waves are emitted from stellar mass black holes with accretion disks. Super massive black holes, since the accretion disk isn’t as hot, tends to peak in the ultraviolet range. • This electromagnetic radiation can be detected and the mass of the unseen companion can be determined. If it is about 3 solar masses or more, than it may be a black hole. • Drawing Credit: A. Hobart, CXC

  12. How to detect black holes- Motion of stars around a black hole • If, in a binary star system, one star seems to orbit an unseen object and the mass is determined to be large enough, then you may have a black hole. • If you observe how stars near the galactic centre move and determine that they must be orbiting something extremely massive, then you may have a super massive black hole. Max-Planck Institute, Germany

  13. How to detect black holes-Gamma ray bursts • Long duration gamma ray bursts are thought to be caused by hyper nova which ejects their outer material to near the speed of light, leaving a core that forms into a black hole. • One thought on the cause of short duration gamma ray bursts is that they are caused by the merger of two neutron stars. However, no one really knows. • Either way, a black hole is associated with these events, so if you detect a gamma ray burst, chances are, there is a black hole there. Credit: The NRAO

  14. How to detect black holes-Hawking radiation • According to Stephen Hawking, black holes emit radiation due to a particle - antiparticle pair production process near the event horizon of a black hole. Real particle appears outside the horizon, antiparticle appear inside the horizon, real particle shoots off into space, antiparticle annihilates inside black hole, black hole loses energy in form of thermal radiation. This is low energy radiation, less than the microwave background of the universe.

  15. Images • Date acquired: March 17th, 2009 from 9:50pm -10:20pm CDT. • Location: Glenlea Astronomical Observatory (GAO). • Telescope: Evans telescope, 40cm, Cassegrain design. • Camera: Apogee CCD Camera, chip size – 1024 X 1024 pixels binned 2 X 2. • Wavelength: Optical. • Exposure time: 26 combined images of 60 s exposure each. • FoV: 6.898’ X 6.980’. • Orientation: North – up, East – right. • Credit: All images not credit were taken by Ben Guest, Todd Pernerowski and Jesse Corley. Final processed image.

  16. Images Final processed image. Faint detail

  17. Images Final processed image. Bright detail

  18. Images Final processed image. High contrast bright detail

  19. Images Final processed image. Log scale, showing both bright and faint detail.

  20. Images Final processed image. Min filter highlighting dead pixels. Radius = 5 pixels.

  21. Images Final processed image. Gauss blurred, contour plot. Grey values: Red-796.6, blue- 739.2, green-681.8, yellow-624.4, orange-567, cyan-495, white-452.0 (border only).

  22. Images Final processed image. Variance filter. Shows a possible X-Ray source. Radius = 10 pixels.

  23. Image Comparisons Camera: Planetary Camera Telescope: Hubble Space Telescope (HST) Location: Earth Orbit. Note: Disk is about 100 ly across. Final processed image. Date: Sometime before June, 1992. Wavelength: Optical. Camera: Planetary Camera Telescope: Hubble Space Telescope (HST) Location: Earth Orbit. H. Ford (JHU/STScI)/FOS IDT/NASA

  24. Image Comparisons Wavelength: X-Ray Exposure time: 4.1 hours (June 20, 2000), 7.4 hours (June 23, 2001) Orientation: North – up, East – right. FoV:Large image: 11.6 x10 arcmin, Inset: about 1.6'x1.5' Final processed image. Date acquired: June 20, 2000 & June 23, 2001 Location: Earth orbit Telescope: Chandra X-Ray Observatory. Camera: Chandra Advanced CCD Imaging Spectrometer (ACIS)

  25. References • Takáts, K, Vinkó, J. 2006. Distance estimate and progenitor characteristics of SN 2005cs in M51. Monthly Notices of the Royal Astronomical Society, Volume 372, Issue 4, pp. 1735-1740. (Abstr.) • Yoshiaki S, Vera R. 2001. ROTATION CURVES OF SPIRAL GALAXIES. Annu. Rev. Astron. Astrophys. 2001. 39: 137-174. (Abstr.) • Messier 51. Last modified: November 4, 2007. http://www.maa.clell.de/Messier/E/m051.html. • Type of Galaxies. Last modified: April 16, 2009. http://www.supernovae.net/nomen.htm. • Audio Podcasts: "Touch the Invisible Sky“ - Chapter 7: Whirlpool Galaxy (M51) . Last Revised: Sept. 19, 2008. http://chandra.harvard.edu/edu/touch/touch_chapter7.html. • NASA's Hubble Space Telescope Resolves a Dark "x" Across the Nucleus of M51. June 8, 1992. http://hubblesite.org/newscenter/archive/releases/1992/17/text/. • Whirlpool Galaxy: High-Energy Activity Heats Up the Whirlpool. Last revised: Feb. 23, 2009. http://chandra.harvard.edu/photo/2002/0158/. • Gamma-Ray Bursts: Introduction to a Mystery. Last Modified: April 16, 2009. http://imagine.gsfc.nasa.gov/docs/science/know_l1/bursts.html. • This research has made use of the SIMBAD database,operated at CDS, Strasbourg, France. • Garfinkle D, Garfinkle R. 2008.Three Steps to the Universe. 4-8:67-155. London: University of Chicago Press.

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