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Interstellar medium
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The distribution of ionized hydrogen (known by astronomers as H II from old spectroscopic terminology) in the parts of the Galactic interstellar medium visible from the Earth's northern hemisphere as observed with the Wisconsin Hα Mapper (Haffner et al. 2003).
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In astronomy, the interstellar medium (ISM) is the matter and radiation that exists in the space between the star systems in a galaxy. This matter includes gas in ionic, atomic, and molecular form, as well as dust and cosmic rays. It fills interstellar space and blends smoothly into the surrounding intergalactic space. The energy that occupies the same volume, in the form of electromagnetic radiation, is the interstellar radiation field.
The interstellar medium is composed of multiple phases, distinguished by whether matter is ionic, atomic, or molecular, and the temperature and density of the matter. The interstellar medium is composed primarily of hydrogen followed by helium with trace amounts of carbon, oxygen, and nitrogen comparatively to hydrogen.[1] The thermal pressures of these phases are in rough equilibrium with one another. Magnetic fields and turbulent motions also provide pressure in the ISM, and are typically more important dynamically than the thermal pressure is.
In all phases, the interstellar medium is extremely tenuous by terrestrial standards. In cool, dense regions of the ISM, matter is primarily in molecular form, and reaches number densities of 106 molecules per cm3 (1 million molecules per cm3). In hot, diffuse regions of the ISM, matter is primarily ionized, and the density may be as low as 10−4 ions per cm3. Compare this with a number density of roughly 1019 molecules per cm3 for air at sea level, and 1010 molecules per cm3 (10 billion molecules per cm3) for a laboratory high-vacuum chamber. By mass, 99% of the ISM is gas in any form, and 1% is dust.[2] Of the gas in the ISM, by number 91% of atoms are hydrogen and 9% are helium, with 0.1% being atoms of elements heavier than hydrogen or helium,[3] known as "metals" in astronomical parlance. By mass this amounts to 70% hydrogen, 28% helium, and 1.5% heavier elements. The hydrogen and helium are primarily a result of primordial nucleosynthesis, while the heavier elements in the ISM are mostly a result of enrichment in the process of stellar evolution.
The ISM plays a crucial role in astrophysics precisely because of its intermediate role between stellar and galactic scales. Stars form within the densest regions of the ISM, molecular clouds, and replenish the ISM with matter and energy through planetary nebulae, stellar winds, and supernovae. This interplay between stars and the ISM helps determine the rate at which a galaxy depletes its gaseous content, and therefore its lifespan of active star formation.
Voyager 1 reached the ISM on August 25, 2012, making it the first artificial object from Earth to do so. Interstellar plasma and dust will be studied until the mission's end in 2025.
Voyager 1 is the first artificial object to reach the ISM
Contents
[hide]
1 Interstellar matter
1.1 The three-phase model
1.2 The atomic hydrogen model
1.3 Structures
1.4 Interaction with interplanetary medium
1.5 Interstellar extinction
2 Heating and cooling
2.1 Heating mechanisms
2.2 Cooling mechanisms
3 Radiowave propagation
4 History of knowledge of interstellar space
5 See also
6 Notes
7 References
8 External links
Interstellar matter[edit]
Table 1 shows a breakdown of the properties of the components of the ISM of the Milky Way.
Table 1: Components of the interstellar medium[3]
Component
Fractional
volume
Scale height
(pc)
Temperature
(K)
Density
(particles/cm3)
State of hydrogen
Primary observational techniques
Molecular clouds < 1% 80 10–20 102–106 molecular Radio and infrared molecular emission and absorption lines
Cold Neutral Medium (CNM) 1–5% 100–300 50–100 20–50 neutral atomic H I 21 cm line absorption
Warm Neutral Medium (WNM) 10–20% 300–400 6000–10000 0.2–0.5 neutral atomic H I 21 cm line emission
Warm Ionized Medium (WIM) 20–50% 1000 8000 0.2–0.5 ionized Hα emission and pulsar dispersion
H II regions < 1% 70 8000 102–104 ionized Hα emission and pulsar dispersion
Coronal gas
Hot Ionized Medium (HIM) 30–70% 1000–3000 106–107 10−4–10−2 ionized
(metals also highly ionized) X-ray emission; absorption lines of highly ionized metals, primarily in the ultraviolet
The three-phase model[edit]
Field, Goldsmith & Habing (1969) put forward the static two phase equilibrium model to explain the observed properties of the ISM. Their modeled ISM consisted of a cold dense phase (T < 300 K), consisting of clouds of neutral and molecular hydrogen, and a warm intercloud phase (T ~ 104 K), consisting of rarefied neutral and ionized gas. McKee & Ostriker (1977) added a dynamic third phase that represented the very hot (T ~ 106 K) gas which had been shock heated by supernovae and constituted most of the volume of the ISM. These phases are the temperatures where heating and cooling can reach a stable equilibrium. Their paper formed the basis for further study over the past three decades. However, the relative proportions of the phases and their subdivisions are still not well known.[3]
The atomic hydrogen model[edit]
This model takes into account only atomic hydrogen : Temperature larger than 3000 K breaks molecules, lower than 50 000 K leaves atoms in their ground state. It is assumed that influence of other atoms (He ...) is negligible. Pressure is assumed very low, so that durations of free paths of atoms are larger than ~ 1 nanosecond duration of light pulses which make ordinary, temporally incoherent light .
In this collisionless gas, Einstein’s theory of coherent light-matter interactions applies, all gas-light interactions are spatially coherent. Suppose that a monochromatic light is pulsed, then scattered by molecules having a quadrupole (Raman) resonance frequency. If “length of light pulses is shorter than all involved time constants” (Lamb (1971)), an “impulsive stimulated Raman scattering (ISRS) ” (Yan, Gamble & Nelson (1985)) works: While light generated by incoherent Raman at a shifted frequency has a phase independent on phase of exciting light, thus generates a new spectral line, coherence between incident and scattered light allows their interference into a single frequency, thus shifts incident frequency. Assume that a star radiates a continuous light spectrum up to X rays. Lyman frequencies are absorbed in this light and pump atoms mainly to first excited state. In this state, hyperfine periods are longer than 1 ns, so that an ISRS “may” redshift light frequency, populating high hyperfine levels. An other ISRS “may” transfer energy from hyperfine levels to thermal electromagnetic waves, so that redshift is permanent. Temperature of a light beam is defined from frequency and spectral radiance by Planck’s formula. As entropy must increase, “may” becomes “does”. However, where a previously absorbed line (first Lyman beta, ...) reaches Lyman alpha frequency, redshifting process stops and all hydrogen lines are strongly absorbed. But the stop is not perfect if there is energy at frequency shifted to Lyman beta frequency, which produces a slow redshift. Successive redshifts separated by Lyman absorptions generate many absorption lines, frequencies of which, deduced from absorption process, obey a law more dependable than Karlsson’s formula.
The previous process excites more and more atoms because a de-excitation obeys Einstein’s law of coherent interactions: Variation dI of radiance I of a light beam along a path dx is dI=BIdx, where B is Einstein amplification coefficient which depends on medium. I is the modulus of Poynting vector of field, absorption occurs for an opposed vector, which corresponds to a change of sign of B. Factor I in this formula shows that intense rays are more amplified than weak ones (competition of modes). Emission of a flare requires a sufficient radiance I provided by random zero point field. After emission of a flare, weak B increases by pumping while I remains close to zero: De-excitation by a coherent emission involves stochastic parameters of zero point field, as observed close to quasars (and in polar auroras).
Structures[edit]
Three-dimensional structure in Pillars of Creation.[4]
The ISM is turbulent and therefore full of structure on all spatial scales. Stars are born deep inside large complexes of molecular clouds, typically a few parsecs in size. During their lives and deaths, stars interact physically with the ISM.
Stellar winds from young clusters of stars (often with giant or supergiant HII regions surrounding them) and shock waves created by supernovae inject enormous amounts of energy into their surroundings, which leads to hypersonic turbulence. The resultant structures – of varying sizes – can be observed, such as stellar wind bubbles and superbubbles of hot gas, seen by X-ray satellite telescopes or turbulent flows observed in radio telescope maps.
The Sun is currently traveling through the Local Interstellar Cloud, a denser region in the low-density Local Bubble.
Interaction with interplanetary medium[edit]
Play media
Short, narrated video about IBEX's interstellar matter observations.
The interstellar medium begins where the interplanetary medium of the Solar System ends. The solar wind slows to subsonic velocities at the termination shock, 90—100 astronomical units from the Sun. In the region beyond the termination shock, called the heliosheath, interstellar matter interacts with the solar wind. Voyager 1, the farthest human-made object from the Earth (after 1998[5]), crossed the termination shock December 16, 2004 and later entered interstellar space when it crossed the heliopause on August 25, 2012, providing the first direct probe of conditions in the ISM (Stone et al. 2005).
Interstellar extinction[edit]
The ISM is also responsible for extinction and reddening, the decreasing light intensity and shift in the dominant observable wavelengths of light from a star. These effects are caused by scattering and absorption of photons and allow the ISM to be observed with the naked eye in a dark sky. The apparent rifts that can be seen in the band of the Milky Way – a uniform disk of stars – are caused by absorption of background starlight by molecular clouds within a few thousand light years from Earth.
Far ultraviolet light is absorbed effectively by the neutral components of the ISM. For example, a typical absorption wavelength of atomic hydrogen lies at about 121.5 nanometers, the Lyman-alpha transition. Therefore, it is nearly impossible to see light emitted at that wavelength from a star farther than a few hundred light years from Earth, because most of it is absorbed during the trip to Earth by intervening neutral hydrogen.
Heating and cooling[edit]
The ISM is usually far from thermodynamic equilibrium. Collisions establish a Maxwell–Boltzmann distribution of velocities, and the 'temperature' normally used to describe interstellar gas is the 'kinetic temperature', which describes the temperature at which the particles would have the observed Maxwell–Boltzmann velocity distribution in thermodynamic equilibrium. However, the interstellar radiation field is typically much weaker than a medium in thermodynamic equilibrium; it is most often roughly that of an A star (surface temperature of ~10,000 K) highly diluted. Therefore, bound levels within an atom or molecule in the ISM are rarely populated according to the Boltzmann formula (Spitzer 1978, § 2.4).
Depending on the temperature, density, and ionization state of a portion of the ISM, different heating and cooling mechanisms determine the temperature of the gas.
Heating mechanisms[edit]
Heating by low-energy cosmic rays
The first mechanism proposed for heating the ISM was heating by low-energy cosmic rays. Cosmic rays are an efficient heating source able to penetrate in the depths of molecular clouds. Cosmic rays transfer energy to gas through both ionization and excitation and to free electrons through Coulomb interactions. Low-energy cosmic rays (a few MeV) are more important because they are far more numerous than high-energy cosmic rays.
Photoelectric heating by grains
The ultraviolet radiation emitted by hot stars can remove electrons from dust grains. The photon is absorbed by the dust grain, and some of its energy is used to overcome the potential energy barrier and remove the electron from the grain. This potential barrier is due to the binding energy of the electron (the work function) and the charge of the grain. The remainder of the photon's energy gives the ejected electron kinetic energy which heats the gas through collisions with other particles. A typical size distribution of dust grains is n(r) ∝ r−3.5, where r is the radius of the dust particle[6]. Assuming this, the projected grain surface area distribution is πr2n(r) ∝ r−1.5. This indicates that the smallest dust grains dominate this method of heating[7].
Photoionization
When an electron is freed from an atom (typically from absorption of a UV photon) it carries kinetic energy away of the order Ephoton − Eionization. This heating mechanism dominates in H II regions, but is negligible in the diffuse ISM due to the relative lack of neutral carbon atoms.
X-ray heating
X-rays remove electrons from atoms and ions, and those photoelectrons can provoke secondary ionizations. As the intensity is often low, this heating is only efficient in warm, less dense atomic medium (as the column density is small). For example, in molecular clouds only hard x-rays can penetrate and x-ray heating can be ignored. This is assuming the region is not near an x-ray source such as a supernova remnant.
Chemical heating
Molecular hydrogen (H2) can be formed on the surface of dust grains when two H atoms (which can travel over the grain) meet. This process yields 4.48 eV of energy distributed over the rotational and vibrational modes, kinetic energy of the H2 molecule, as well as heating the dust grain. This kinetic energy, as well as the energy transferred from de-excitation of the hydrogen molecule through collisions, heats the gas.
Grain-gas heating
Collisions at high densities between gas atoms and molecules with dust grains can transfer thermal energy. This is not important in HII regions because UV radiation is more important. It is also not important in diffuse ionized medium due to the low density. In the neutral diffuse medium grains are always colder, but do not effectively cool the gas due to the low densities.
Grain heating by thermal exchange is very important in supernova remnants where densities and temperatures are very high.
Gas heating via grain-gas collisions is dominant deep in giant molecular clouds (especially at high densities). Far infrared radiation penetrates deeply due to the low optical depth. Dust grains are heated via this radiation and can transfer thermal energy during collisions with the gas. A measure of efficiency in the heating is given by the accommodation coefficient:
α = T 2 − T T d − T {\displaystyle \alpha ={\frac {T_{2}-T}{T_{d}-T}}}
where T is the gas temperature, Td the dust temperature, and T2 the post-collision temperature of the gas atom or molecule. This coefficient was measured by (Burke & Hollenbach 1983) as α = 0.35.
Other heating mechanisms
A variety of macroscopic heating mechanisms are present including:
Gravitational collapse of a cloud
Supernova explosions
Stellar winds
Expansion of H II regions
Magnetohydrodynamic waves created by supernova remnants
Cooling mechanisms[edit]
Fine structure cooling
The process of fine structure cooling is dominant in most regions of the Interstellar Medium, except regions of hot gas and regions deep in molecular clouds. It occurs most efficiently with abundant atoms having fine structure levels close to the fundamental level such as: C II and O I in the neutral medium and O II, O III, N II, N III, Ne II and Ne III in H II regions. Collisions will excite these atoms to higher levels, and they will eventually de-excite through photon emission, which will carry the energy out of the region.
Cooling by permitted lines
At lower temperatures, more levels than fine structure levels can be populated via collisions. For example, collisional excitation of the n = 2 level of hydrogen will release a Ly-α photon upon de-excitation. In molecular clouds, excitation of rotational lines of CO is important. Once a molecule is excited, it eventually returns to a lower energy state, emitting a photon which can leave the region, cooling the cloud.
Radiowave propagation[edit]
Atmospheric attenuation in dB/km as a function of frequency over the EHF band. Peaks in absorption at specific frequencies are a problem, due to atmosphere constituents such as water vapor (H2O) and carbon dioxide (CO2).
Radio waves from ≈10 kHz (very low frequency) to ≈300 GHz (extremely high frequency) propagate differently in interstellar space than on the Earth's surface. There are many sources of interference and signal distortion that do not exist on Earth. A great deal of radio astronomy depends on compensating for the different propagation effects to uncover the desired signal.[8][9]
History of knowledge of interstellar space[edit]
Herbig–Haro 110 object ejects gas through interstellar space.[10]
The nature of the interstellar medium has received the attention of astronomers and scientists over the centuries, and understanding of the ISM has developed. However, they first had to acknowledge the basic concept of "interstellar" space. The term appears to have been first used in print by Bacon (1626, § 354–5): "The Interstellar Skie.. hath .. so much Affinity with the Starre, that there is a Rotation of that, as well as of the Starre." Later, natural philosopher Robert Boyle (1674) discussed "The inter-stellar part of heaven, which several of the modern Epicureans would have to be empty."
Before modern electromagnetic theory, early physicists postulated that an invisible luminiferous aether existed as a medium to carry lightwaves. It was assumed that this aether extended into interstellar space, as Patterson (1862) wrote, "this efflux occasions a thrill, or vibratory motion, in the ether which fills the interstellar spaces."
The advent of deep photographic imaging allowed Edward Barnard to produce the first images of dark nebulae silhouetted against the background star field of the galaxy, while the first actual detection of cold diffuse matter in interstellar space was made by Johannes Hartmann in 1904[11] through the use of absorption line spectroscopy. In his historic study of the spectrum and orbit of Delta Orionis, Hartmann observed the light coming from this star and realized that some of this light was being absorbed before it reached the Earth. Hartmann reported that absorption from the "K" line of calcium appeared "extraordinarily weak, but almost perfectly sharp" and also reported the "quite surprising result that the calcium line at 393.4 nanometres does not share in the periodic displacements of the lines caused by the orbital motion of the spectroscopic binary star". The stationary nature of the line led Hartmann to conclude that the gas responsible for the absorption was not present in the atmosphere of Delta Orionis, but was instead located within an isolated cloud of matter residing somewhere along the line-of-sight to this star. This discovery launched the study of the Interstellar Medium.
In the series of investigations, Viktor Ambartsumian introduced the now commonly accepted notion that interstellar matter occurs in the form of clouds.[12]
Following Hartmann's identification of interstellar calcium absorption, interstellar sodium was detected by Heger (1919) through the observation of stationary absorption from the atom's "D" lines at 589.0 and 589.6 nanometres towards Delta Orionis and Beta Scorpii.
Subsequent observations of the "H" and "K" lines of calcium by Beals (1936) revealed double and asymmetric profiles in the spectra of Epsilon and Zeta Orionis. These were the first steps in the study of the very complex interstellar sightline towards Orion. Asymmetric absorption line profiles are the result of the superposition of multiple absorption lines, each corresponding to the same atomic transition (for example the "K" line of calcium), but occurring in interstellar clouds with different radial velocities. Because each cloud has a different velocity (either towards or away from the observer/Earth) the absorption lines occurring within each cloud are either Blue-shifted or Red-shifted (respectively) from the lines' rest wavelength, through the Doppler Effect. These observations confirming that matter is not distributed homogeneously were the first evidence of multiple discrete clouds within the ISM.
This light-year-long knot of interstellar gas and dust resembles a caterpillar.[13]
The growing evidence for interstellar material led Pickering (1912) to comment that "While the interstellar absorbing medium may be simply the ether, yet the character of its selective absorption, as indicated by Kapteyn, is characteristic of a gas, and free gaseous molecules are certainly there, since they are probably constantly being expelled by the Sun and stars."
The same year Victor Hess's discovery of cosmic rays, highly energetic charged particles that rain onto the Earth from space, led others to speculate whether they also pervaded interstellar space. The following year the Norwegian explorer and physicist Kristian Birkeland wrote: "It seems to be a natural consequence of our points of view to assume that the whole of space is filled with electrons and flying electric ions of all kinds. We have assumed that each stellar system in evolutions throws off electric corpuscles into space. It does not seem unreasonable therefore to think that the greater part of the material masses in the universe is found, not in the solar systems or nebulae, but in 'empty' space" (Birkeland 1913).
Thorndike (1930) noted that "it could scarcely have been believed that the enormous gaps between the stars are completely void. Terrestrial aurorae are not improbably excited by charged particles emitted by the Sun. If the millions of other stars are also ejecting ions, as is undoubtedly true, no absolute vacuum can exist within the galaxy."
In September 2012, NASA scientists reported that polycyclic aromatic hydrocarbons (PAHs), subjected to interstellar medium (ISM) conditions, are transformed, through hydrogenation, oxygenation and hydroxylation, to more complex organics – "a step along the path toward amino acids and nucleotides, the raw materials of proteins and DNA, respectively".[14][15] Further, as a result of these transformations, the PAHs lose their spectroscopic signature which could be one of the reasons "for the lack of PAH detection in interstellar ice grains, particularly the outer regions of cold, dense clouds or the upper molecular layers of protoplanetary disks."[14][15]
In February 2014, NASA announced a greatly upgraded database for tracking polycyclic aromatic hydrocarbons (PAHs) in the universe. According to scientists, more than 20% of the carbon in the universe may be associated with PAHs, possible starting materials for the formation of life. PAHs seem to have been formed shortly after the Big Bang, are widespread throughout the universe, and are associated with new stars and exoplanets.[16]
See also[edit]
Astronomy portal
Solar System portal
Space portal
Astrophysical maser
Diffuse interstellar band
Fossil stellar magnetic field
Heliosphere
List of interstellar and circumstellar molecules
List of plasma physics articles
Molecular Clouds
Photodissociation region
Notes[edit]
Jump up ^ Herbst, Eric (1995). "Chemistry in The Interstellar Medium". Annual Review of Physical Chemistry. Bibcode:1995ARPC...46...27H. doi:10.1146/annurev.pc.46.100195.000331. Retrieved 2014-10-24.
Jump up ^ Boulanger, F.; Cox, P.; Jones, A. P. (2000). "Course 7: Dust in the Interstellar Medium". In F. Casoli; J. Lequeux; F. David. Infrared Space Astronomy, Today and Tomorrow. p. 251. Bibcode:2000isat.conf..251B.
^ Jump up to: a b c Ferriere (2001)
Jump up ^ "The Pillars of Creation Revealed in 3D". European Southern Observatory. 30 April 2015. Retrieved 14 June 2015.
Jump up ^ "Voyager: Fast Facts". Jet Propulsion Laboratory.
Jump up ^ Mathis, J.S.; Rumpl, W.; Nordsieck, K.H. "The size distribution of interstellar grains". Astrophysical Journal. 217: 425. Bibcode:1977ApJ...217..425M. doi:10.1086/155591.
Jump up ^ Weingartner, J.C.; Draine, B.T. "Photoelectric Emission from Interstellar Dust: Grain Charging and Gas Heating". Astrophysical Journal Supplement Series. 134: 263. arXiv:astro-ph/9907251  . Bibcode:2001ApJS..134..263W. doi:10.1086/320852.
Jump up ^ Samantha Blair. "Interstellar Medium Interference (video)". SETI Talks.
Jump up ^ "Voyager 1 Experiences Three Tsunami Waves in Interstellar Space (video)". JPL.
Jump up ^ "A geyser of hot gas flowing from a star". ESA/Hubble Press Release. Retrieved 3 July 2012.
Jump up ^ Asimov, Isaac, Asimov's Biographical Encyclopedia of Science and Technology (2nd ed.)
Jump up ^ S. Chandrasekhar (1989), "To Victor Ambartsumian on his 80th birthday", Journal of Astrophysics and Astronomy, 18: 3, Bibcode:1988Ap.....29..408C, doi:10.1007/BF01005852
Jump up ^ "Hubble sees a cosmic caterpillar". Image Archive. ESA/Hubble. Retrieved 9 September 2013.
^ Jump up to: a b Staff (September 20, 2012), NASA Cooks Up Icy Organics to Mimic Life's Origins, Space.com, retrieved September 22, 2012
^ Jump up to: a b Gudipati, Murthy S.; Yang, Rui (September 1, 2012), "In-Situ Probing Of Radiation-Induced Processing Of Organics In Astrophysical Ice Analogs—Novel Laser Desorption Laser Ionization Time-Of-Flight Mass Spectroscopic Studies", The Astrophysical Journal Letters, 756 (1): L24, Bibcode:2012ApJ...756L..24G, doi:10.1088/2041-8205/756/1/L24, retrieved September 22, 2012
Jump up ^ Hoover, Rachel (February 21, 2014). "Need to Track Organic Nano-Particles Across the Universe? NASA's Got an App for That". NASA. Retrieved February 22, 2014.
References[edit]
Bacon, Francis (1626), Sylva (3545 ed.)
Beals, C. S. (1936), "On the interpretation of interstellar lines", Monthly Notices of the Royal Astronomical Society, 96: 661, Bibcode:1936MNRAS..96..661B, doi:10.1093/mnras/96.7.661
Birkeland, Kristian (1913), "Polar Magnetic Phenomena and Terrella Experiments", The Norwegian Aurora Polaris Expedition, 1902-03 (section 2), New York: Christiania (now Oslo), H. Aschelhoug & Co., p. 720 out-of-print, full text online
Boyle, Robert (1674), The Excellency of Theology Compar'd with Natural Philosophy, ii. iv., p. 178
Burke, J. R.; Hollenbach, D.J. (1983), "The gas-grain interaction in the interstellar medium – Thermal accommodation and trapping", Astrophysical Journal, 265: 223, Bibcode:1983ApJ...265..223B, doi:10.1086/160667
Dyson, J. (1997), Physics of the Interstellar Medium, London: Taylor & Francis
Field, G. B.; Goldsmith, D. W.; Habing, H. J. (1969), "Cosmic-Ray Heating of the Interstellar Gas", Astrophysical Journal, 155: L149, Bibcode:1969ApJ...155L.149F, doi:10.1086/180324
Ferriere, K. (2001), "The Interstellar Environment of our Galaxy", Reviews of Modern Physics, 73 (4): 1031–1066, arXiv:astro-ph/0106359  , Bibcode:2001RvMP...73.1031F, doi:10.1103/RevModPhys.73.1031
Haffner, L. M.; Reynolds, R. J.; Tufte, S. L.; Madsen, G. J.; Jaehnig, K. P.; Percival, J. W. (2003), "The Wisconsin Hα Mapper Northern Sky Survey", Astrophysical Journal Supplement, 145 (2): 405, arXiv:astro-ph/0309117  , Bibcode:2003ApJS..149..405H, doi:10.1086/378850 . The Wisconsin Hα Mapper is funded by the National Science Foundation.
Heger, Mary Lea (1919), "Stationary Sodium Lines in Spectroscopic Binaries", Publications of the Astronomical Society of the Pacific, 31 (184): 304, Bibcode:1919PASP...31..304H, doi:10.1086/122890
Lamb G. L. Jr. “Analytical description of ultra-short optical pulse propagation in a resonant medium”, Rev. Mod. Phys., 43, 99-124.
Lequeux, J. The Interstellar Medium. Springer 2005.
McKee, C. F.; Ostriker, J. P. (1977), "A theory of the interstellar medium – Three components regulated by supernova explosions in an inhomogeneous substrate", Astrophysical Journal, 218: 148, Bibcode:1977ApJ...218..148M, doi:10.1086/155667
Patterson, Robert Hogarth (1862), "Colour in nature and art", Essays in History and Art, 10 Reprinted from Blackwood's Magazine.
Pickering, W. H. (1912), "The Motion of the Solar System relatively to the Interstellar Absorbing Medium", Monthly Notices of the Royal Astronomical Society, 72: 740, Bibcode:1912MNRAS..72..740P, doi:10.1093/mnras/72.9.740
Spitzer, L. (1978), Physical Processes in the Interstellar Medium, Wiley, ISBN 0-471-29335-0
Stone, E. C.; Cummings, A. C.; McDonald, F. B.; Heikkila, B. C.; Lal, N.; Webber, W. R. (2005), "Voyager 1 Explores the Termination Shock Region and the Heliosheath Beyond", Science, 309 (5743): 2017–20, Bibcode:2005Sci...309.2017S, doi:10.1126/science.1117684, PMID 16179468
Thorndike, S. L. (1930), "Interstellar Matter", Publications of the Astronomical Society of the Pacific, 42 (246): 99, Bibcode:1930PASP...42...99T, doi:10.1086/124007
Yan, Y. X.; Gamble, E.B. Jr.; Nelson K. A. (1985), “Impulsive Stimulated Scattering: General Importance in Femto-second Laser Pulse Interactions with Matter and Spectroscopic Applications”, J. Chem. Phys., 83, 3591–5399.
External links[edit]
Freeview Video 'Chemistry of Interstellar Space' William Klemperer, Harvard University. A Royal Institution Discourse by the Vega Science Trust.
The interstellar medium: an online tutorial
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Molecules detected in outer space
Molecules
Diatomic
Aluminium monochloride
Aluminium monofluoride
Aluminium monoxide
Argonium
Carbon monophosphide
Carbon monosulfide
Carbon monoxide
Carborundum
Cyanogen radical
Diatomic carbon
Fluoromethylidynium
Hydrogen chloride
Hydrogen fluoride
Hydrogen (molecular)
Hydroxyl radical
Iron(II) oxide
Magnesium monohydride cation
Methylidyne radical
Nitric oxide
Nitrogen (molecular)
Nitrogen monohydride
Nitrogen sulfide
Oxygen (molecular)
Phosphorus monoxide
Phosphorus mononitride
Potassium chloride
Silicon carbide
Silicon mononitride
Silicon monoxide
Silicon monosulfide
Sodium chloride
Sodium iodide
Sulfur monohydride
Sulfur monoxide
Titanium oxide

Triatomic
Aluminium hydroxide
Aluminium isocyanide
Amino radical
Carbon dioxide
Carbonyl sulfide
CCP radical
Chloronium
Diazenylium
Dicarbon monoxide
Disilicon carbide
Ethynyl radical
Formyl radical
Hydrogen cyanide (HCN)
Hydrogen isocyanide (HNC)
Hydrogen sulfide
Hydroperoxyl
Iron cyanide
Isoformyl
Magnesium cyanide
Magnesium isocyanide
Methylene radical
N2H+
Nitrous oxide
Nitroxyl
Ozone
Phosphaethyne
Potassium cyanide
Protonated molecular hydrogen
Sodium cyanide
Sodium hydroxide
Silicon carbonitride
c-Silicon dicarbide
Silicon naphthalocyanine
Sulfur dioxide
Thioformyl
Thioxoethenylidene
Titanium dioxide
Tricarbon
Water
Four
atoms
Acetylene
Ammonia
Cyanic acid
Cyanoethynyl
Cyclopropynylidyne
Formaldehyde
Fulminic acid
HCCN
Hydrogen peroxide
Hydromagnesium isocyanide
Isocyanic acid
Isothiocyanic acid
Ketenyl
Methylene amidogen
Methyl radical
Propynylidyne
Protonated carbon dioxide
Protonated hydrogen cyanide
Silicon tricarbide
Thioformaldehyde
Tricarbon monoxide
Tricarbon sulfide
Thiocyanic acid
Five
atoms
Ammonium ion
Butadiynyl
Carbodiimide
Cyanamide
Cyanoacetylene
Cyanoformaldehyde
Cyanomethyl
Cyclopropenylidene
Formic acid
Isocyanoacetylene
Ketene
Methane
Methoxy radical
Methylenimine
Propadienylidene
Protonated formaldehyde
Protonated formaldehyde
Silane
Silicon-carbide cluster
Six
atoms
Acetonitrile
Cyanobutadiynyl radical
E-Cyanomethanimine
Cyclopropenone
Diacetylene
Ethylene
Formamide
HC4N
Ketenimine
Methanethiol
Methanol
Methyl isocyanide
Pentynylidyne
Propynal
Protonated cyanoacetylene
Seven
atoms
Acetaldehyde
Acrylonitrile
Vinyl cyanide
Cyanodiacetylene
Ethylene oxide
Hexatriynyl radical
Methylacetylene
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LCCN: sh85067526
GND: 4162140-2
NDL: 00570319
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Crazy Eyes (character)
From Wikipedia, the free encyclopedia
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Suzanne "Crazy Eyes" Warren
Orange Is the New Black character
Uzo Aduba as Suzanne "Crazy Eyes" Warren in a promotional poster for season 2 of Orange Is the New Black
First appearance
"I Wasn't Ready"
Season 1, episode 1
July 11, 2013
Portrayed by
Uzo Aduba
Eden Wiggins (at age 10)
Taliyah Whitaker (at age 5)
Information
Significant other(s)
Maureen Kukudio (ex-girlfriend)
Parents
Pat Warren (adoptive mother)
Dennis Warren (adoptive father)
Suzanne "Crazy Eyes" Warren is a fictional character played by Uzo Aduba on the Netflix series Orange Is the New Black. Warren is portrayed as intelligent, but lacking in social skills, and prone to spiral into emotional outbursts when agitated. The character is the only role that has received Emmy Award recognition both in the comedy and drama genres from the same show and only the second character to earn Emmy recognition in both genres. Aduba won the Emmy Award for Outstanding Guest Actress in a Comedy Series as well as the Critics' Choice Television Award for Best Guest Performer in a Comedy Series for her season one performance. She received the Emmy Award for Outstanding Supporting Actress in a Drama Series as well as the Screen Actors Guild Award for Outstanding Performance by a Female Actor in a Comedy Series for her season two performance. Her season three performance again won Screen Actors Guild Award for Outstanding Performance by a Female Actor in a Comedy Series. She is a recurring character in season one and a regular character beginning with season two.[1]
Contents
[hide]
1 Appearance
2 Storylines
2.1 Season 1
2.2 Season 2
2.3 Season 3
2.4 Season 4
2.5 Season 5
3 Critical commentary
4 See also
5 References
Appearance[edit]
In season one, Aduba is credited for 11 of the 13 episodes (not the first or seventh), although she appears in the first episode via footage filmed from another episode.[2][3]
In season two, episode three ("Hugs Can Be Deceiving"), Eden Wiggins,and Taliyah Whitaker portray the 10-year-old and 5-year-old versions of Warren.[4] Throughout the first two seasons, it is shown that Warren aspires "to be included" and "to make friends and be valued".[5] The character is known for her bantu knots, an awkward grin, and her crazy eyes.[6][7]
Storylines[edit]
This section needs additional citations for verification. Please help improve this article by adding citations to reliable sources. Unsourced material may be challenged and removed. (June 2017) (Learn how and when to remove this template message)
Season 1[edit]
Suzanne is fixated on Piper Chapman (Taylor Schilling) at the beginning of the season.[8] When Chapman, who has offended prison matriarch Red (Kate Mulgrew), seems hopelessly isolated, Suzanne is the only inmate not too intimidated to help her. She helps Chapman by getting jalapeños, so she can put them in a medicinal lotion for Red's sore back, and Red forgives Chapman. Suzanne nicknames Chapman "Dandelion", because of her blonde hair and puts in a request to become Chapman's bunkmate. Nonetheless, Chapman resists her advances.[9][10][11] As a result, Suzanne urinates on the floor in Chapman's bunk quarters.[12] In episode 9, "Fucksgiving", her white adoptive parents, Pat and Dennis Warren, are introduced.[13][14]
Season 2[edit]
As she rebounds from her unrequited love for Chapman, Suzanne is befriended by veteran inmate Yvonne "Vee" Parker (Lorraine Toussaint) as Vee develops her powerbase in the prison. Vee takes advantage of Suzanne's desperation for affection, and Suzanne becomes Vee's fanatically loyal right-hand woman.[15] Suzanne serves Vee as muscle, even beating up her friend Poussey Washington (Samira Wiley) on Vee's orders.[16] When Vee attacks prison matriarch Galina "Red" Reznikov (Kate Mulgrew) and puts her in the hospital ward, she manipulates Suzanne into believing that she committed the crime. Suzanne gives a statement to prison officials confessing to the attack, but inmate counselor Sam Healy (Michael J. Harney) produces evidence that exonerates her. When she realizes that Vee used her, she breaks into tears.
In episode 3, "Hugs Can Be Deceiving", Suzanne's backstory is revealed via a flashback. She was adopted by white parents and raised in the suburbs, but her mental instability alienated her classmates and their parents alike. Her adoptive mother pushed her to excel at everything she did to prove that she was as good as everyone else; ironically, the constant pressure only made Suzanne's psychological problems worse. In the same episode, it is revealed that Suzanne had run outside and knocked Chapman unconscious after Chapman had beaten Tiffany "Pennsatucky" Doggett (Taryn Manning) unconscious at the end of season 1.[17]
Season 3[edit]
In season 3, Taystee has her hands full trying to control Suzanne, who is still grieving Vee's death and is unstable, prone to losing her temper and constantly fighting with Poussey. Eventually, she turns to new prison counsellor Berdie Rogers's drama class. There, she begins writing a surrealistic science-fiction erotica series called "The Time Hump Chronicles" which, although considered obscene and strange by both Rogers and Taystee, becomes an instant hit amongst the inmates. Although they prove to be therapeutic for her mental health, Suzanne becomes stressed and irritated with the constant harassment by the other inmates for more material, the persistent ideas that are being floated past her and the fan-fiction that is left at her bunk or lying around. Soon, some of the extracts find their way into the hands of the COs, resulting in Officer Donaldson being mocked by both his colleagues and the inmates alike upon the realization that he is the inspiration for one of the characters. This leads to Rogers' suspension. Meanwhile, Suzanne is taken by surprise when she discovers that one of her more prolific fans, Maureen Kukudio, is actually interested in her romantically. Suzanne seeks advice from Lorna about how to respond; she admits she finds Maureen attractive, but she has never had a girlfriend before and subsequently feels she must back away from a sexual liaison. In the season finale, Suzanne assists Poussey and Taystee in caring for Brook Soso, whom they discover unconscious from a drug overdose, and develops a closer bond with Maureen in the final scene, owing to a misunderstanding over a turtle that bites Maureen's foot.[18]
Season 4[edit]
In season 4 it is revealed that Suzanne's crime was kidnapping and accidental manslaughter of a child she grew friendly with while working as a store greeter.[19] Believing that she and the boy were simply being friends, she did not realize the implications of her actions when she came across him playing in the park and invited him to her apartment for ice cream and video games. The boy went willingly, but soon became frightened and wanted to call his dad. While Suzanne is out of the room preparing for what she plans as more fun, he calls 911. Suzanne becomes agitated as she tells him that 911 should only be called when there is an emergency. The child panics and tries to get away. He goes onto the fire escape and falls to his death. It is mentioned that she took a plea deal. When the inmates take advantage of a temporary lack of security and enjoy the nearby lake and woods, Kukudio insists that she and Suzanne run away together. Suzanne refuses and their relationship becomes rocky. In "People Persons", CO Humphrey commands the two of them to fight. Suzanne rejects this but Maureen, who wants to fight, provokes her by launching into a stream of insults. Suzanne fully retaliates by throwing Maureen to the ground and beating her repeatedly, until the Dominicans pull her off. This fight leads her to extreme guilt and a wish to punish herself. She demonstrates this especially when a peaceful protest in the jail cafeteria turns into a chaotic scene and Poussey Washington dies by suffocation. Whilst the inmates grieve over her death, Suzanne believes that Poussey is alive and tries numerous times to suffocate herself. Finally, she is sent to Medical and is placed in a bed next to Kukudio.
Season 5[edit]
In season five, Suzanne continues to recover from her injuries and also goes out of her way to help Maureen, whose injuries are severe. She continues to believe that Poussey's spirit is trying to talk to her and performs a seance on the spot in the cafeteria where Poussey died. Lorna and Nicky take over the dispensation of meds; Lorna refuses to give Suzanne hers, pressuring her to believe she no longer needs them. As a result, Suzanne's grasp on reality soon spirals out of control, especially when she tears down fiberboard in the dorm ceiling, trying to find "heaven". Cindy intervenes but, not knowing the correct prescriptions, feeds Suzanne lithium instead. Suzanne becomes catatonic but is subsequently revived by an epipen.
Critical commentary[edit]
According to Tom Meltzer of The Guardian, "Shakespeare-quoting loner 'Crazy Eyes' invites pity, shock, reproach and belly-laughs in equal measure."[20] The Huffington Post Canada entertainment editor Chris Jancelewicz, noted that after the first six episodes of season two, he was impressed by this appropriately nicknamed character: "Girl is crazy, and Aduba is genuinely frightening in the role. You can't tell if she's harmless or secretly plotting Piper's death".[21]
Aduba won Outstanding Guest Actress in a Comedy Series at the 66th Primetime Creative Arts Emmy Awards as well as Best Guest Performer in a Comedy Series at the 4th Critics' Choice Television Awards and was nominated for Best Supporting Actress – Series, Miniseries or Television Film at the 18th Satellite Awards for her season 1 performance.[22][23][24]
Aduba's season 2 performance earned her the Outstanding Performance by a Female Actor in a Comedy Series at the 21st Screen Actors Guild Awards and a nomination Best Supporting Actress – Series, Miniseries or Television Film at the 72nd Golden Globe Awards.[25][26][27] At the 67th Primetime Emmy Awards, due to recent rule changes, the show was forced to compete as a drama series rather than a comedy one and Aduba was nominated and won for Outstanding Supporting Actress in a Drama Series.[28] Previously, Lou Grant played by Ed Asner was the only character for whom an actor had won both drama and comedy Emmy recognition (but in different shows).[29] She also earned a nomination at the 46th NAACP Image Awards for Outstanding Actress in a Comedy Series.[30]
Aduba's season 3 performance earned another Outstanding Performance by a Female Actor in a Comedy Series win for the 22nd Screen Actors Guild Awards.[31] She earned a second nomination for Outstanding Actress in a Comedy Series at the 47th NAACP Image Awards.[32] She also earned a Best Supporting Actress – Series, Miniseries or Television Film at the 73rd Golden Globe Awards.[33]
At the 69th Primetime Emmy Awards, Aduba was again nominated for the Primetime Emmy Award for Outstanding Supporting Actress in a Drama Series.[34]
See also[edit]
List of Orange Is the New Black characters
References[edit]
Jump up ^ Andreeva, Nellie (August 8, 2013). "Uzo Aduba Upped To Regular On 'Orange Is The New Black', Steven Culp In 'Revolution'". Deadline.com. Retrieved September 5, 2014.
Jump up ^ Kohan, Jenji (writer/creator); Herrmann, Tara (producer); Burley, Mark (producer) (May 13, 2014). Orange Is the New Black: Season 1 – "I Wasn't Ready" audio commentary (Blu-ray). Lionsgate. Event occurs at 37:00–37:30.
Jump up ^ "Uzo Aduba". Internet Movie Database. Retrieved June 12, 2015.
Jump up ^ "Orange is the New Black Season 2 Episode 3: Hugs Can Be Deceiving". TV.com. Retrieved September 5, 2014.
Jump up ^ Potts, Kimberly (June 18, 2014). "The 10 Best 'Orange Is the New Black' Character Backstories". Yahoo! TV. Retrieved September 5, 2014.
Jump up ^ White, Chelsea F.C. (October 2, 2013). "Spot the difference! Orange Is The New Black star Taylor Schilling brings the real Piper Chapman as her red carpet date". Daily Mail. Retrieved October 4, 2014.
Jump up ^ Fitzgerald, Sean (June 23, 2014). "'Orange is the New Black': Meet Crazy Eyes". Toronto Sun. Retrieved October 23, 2014.
Jump up ^ Leopold, Todd (June 6, 2014). "'Orange is the New Black': Five things to expect from season 2". CNN. Retrieved September 6, 2014.
Jump up ^ Hooton, Christopher (June 4, 2014). "Orange Is The New Black: Season 1 recap ahead of the new episodes". The Independent. Retrieved September 6, 2014.
Jump up ^ Schaefer, Megan (June 3, 2014). "'Orange Is The New Black' Season 1 Recap: Everything To Know Before The Season 2 Premiere". International Business Times. Retrieved September 6, 2014.
Jump up ^ Foster, Lewis (June 19, 2014). "Visual Summary: Orange Is The New Black Season 1". Paste. Retrieved September 6, 2014.
Jump up ^ O'Sullivan, Erin (August 14, 2013). "Orange Is The New Black: Uzo Aduba (Suzanne Warren) Promoted To Series Regular". Access Hollywood. Retrieved September 6, 2014.
Jump up ^ Henderson, Danielle (August 16, 2013). "Orange Is the New Black Episode Nine Recap: We Finally Experience the SHU". Vulture. Retrieved September 6, 2014.
Jump up ^ "Orange is the New Black Season 1 Episode 9: F*cksgiving: Episode Cast & Crew". TV.com. Retrieved September 6, 2014.
Jump up ^ Reed, Alex (July 22, 2014). "'Orange Is the New Black' Star Uzo Aduba on 'Crazy Eyes': 'People Underestimate Her' (Video)". The Wrap. Retrieved September 6, 2014.
Jump up ^ Surette, Tim. "Orange Is the New Black Season 2 Review, Part 2 (Episodes 7-13): Fight the Power". TV.com. Retrieved September 6, 2014.
Jump up ^ Surette, Tim. "Orange Is the New Black Season 2 Review, Part 1 (Episodes 1–6): Conflict Over Community". TV.com. Retrieved September 6, 2014.
Jump up ^ http://www.bustle.com/articles/90452-who-is-crazy-eyes-love-interest-on-orange-is-the-new-black-emily-althaus-character-has
Jump up ^ Harnick, Chris (June 18, 2016). "Orange Is the New Black Reveals Crazy Eyes' Tragic Crime". ENews. Retrieved 18 September 2017.
Jump up ^ Meltzer, Tom (December 17, 2013). "The best TV of 2013: No 6 – Orange is the New Black (Netflix): The US prison drama – Netflix's most-watched show of the year – is a binge-watcher's dream: moreish and full of surprises". The Guardian. Retrieved October 5, 2014.
Jump up ^ Jancelewicz, Chris (July 3, 2014). "Orange Is The New Black Review: Time Behind Bars Shouldn't Be This Fun". The Huffington Post Canada. Retrieved October 6, 2014.
Jump up ^ "Primetime Emmy Awards 2014: The winners list". CNN. August 26, 2014. Retrieved September 4, 2014.
Jump up ^ "The International Press Academy Announces Nominations For The 18th Annual Satellite Awards". PR Newswire. December 2, 2013. Retrieved September 5, 2014.
Jump up ^ Atkinson, Kate (June 19, 2014). "Critics' Choice TV Awards: The winners list". Entertainment Weekly. Retrieved September 5, 2014.
Jump up ^ Leeds, Sarene (January 26, 2015). "SAG Awards: The Complete 2015 Winners List". The Wall Street Journal. Retrieved January 27, 2015.
Jump up ^ Keegan, Rebecca (January 26, 2015). "SAG Awards 2015: 'Birdman' feathers its nest as Oscars nears". Los Angeles Times. Retrieved January 27, 2015.
Jump up ^ Mitovich, Matt Webb (December 11, 2014). "Golden Globes: Fargo, True Detective Lead Nominations; Jane the Virgin, Transparent Score Multiple Nods". TVLine. Retrieved December 11, 2014.
Jump up ^ "Emmy Awards 2015: The complete winners list". CNN. September 21, 2015. Retrieved September 21, 2015.
Jump up ^ Donnelly, Matt (September 20, 2015). "Emmy Winner Uzo Aduba Is, in Fact, the New Ed Asner". TheWrap. Retrieved September 24, 2015.
Jump up ^ Washington, Arlene (February 6, 2015). "NAACP Image Awards: The Winners". The Hollywood Reporter. Retrieved June 16, 2016.
Jump up ^ "SAG Awards: The Complete Winners List". The Hollywood Reporter. January 30, 2016. Retrieved February 3, 2016.
Jump up ^ "'Straight Outta Compton,' 'Empire,' Michael B. Jordan Top NAACP Image Awards". Variety. February 5, 2016. Retrieved June 16, 2016.
Jump up ^ "Golden Globes 2016: Complete list of winners and nominees". Los Angeles Times. January 10, 2016. Retrieved July 21, 2016.
Jump up ^ "The complete list of 2017 Emmy winners and nominees". Los Angeles Times. September 17, 2017. Retrieved September 20, 2017.
[hide]
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Orange Is the New Black
Characters
Piper Chapman
Alex Vause
Crazy Eyes
Nicky Nichols
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Lorna Morello
Miss Rosa
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Seasons
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"Lesbian Request Denied"
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5
Related
Piper Kerman
Orange Is the New Black: My Year in a Women's Prison
"You've Got Time"
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