Crab Supernova Rock Art

2015 ◽  
Vol 1 (2) ◽  
pp. 167-197 ◽  
Author(s):  
E. C. Krupp
Keyword(s):  
New Mexico ◽  
Critical Review ◽  
Crab Nebula ◽  
Rock Art ◽  
Supernova Explosion ◽  
American Southwest ◽  
The Sun ◽  
Detailed Evaluation ◽  
The Crab Nebula

“Star” and crescent combinations in rock art in the American Southwest were first interpreted in 1955 as eyewitness depictions of the 1054 AD supernova explosion that produced the Crab nebula. While the Crab nebula is visible only telescopically, the event that generated it was brilliant, and for a time, only the sun and moon were brighter. Additional Crab supernova candidates in California and Southwest rock art were suggested 20 years later, and they included Chaco Canyon’s Penasco Blanco pictograph panel, which became the poster child for Crab supernova rock art and is now called “Supernova” on signage at the site. By 1979, a list of 21 Crab supernova rock art sites was assembled, and the inventory has continued to expand more slowly since then. This critical review of the supernova interpretation of star/crescent rock art, the product of 35 years of fieldwork, required an independent re-examination of all of the primary sites in person. That enterprise has already demonstrated that the Tenabo, New Mexico panel does not illustrate the Crab supernova and that the two Arizona sites on which the entire supernova rock art premise is based (White Mesa and “Navaho Canyon”) are unlikely records of the event. This detailed evaluation of the primary proposed star/crescent images indicates none is a satisfactory portrayal of the striking 1054 AD supernova.

80 MHz Observations of the Coronal Broadening of the Crab Nebula

1970 ◽  
Vol 1 (7) ◽  
pp. 319-320 ◽  
Author(s):  
J. R. Harries ◽  
R. G. Blesing ◽  
P. A. Dennison
Keyword(s):  
Interplanetary Medium ◽  
Crab Nebula ◽  
Angular Size ◽  
Space Vehicles ◽  
Radio Sources ◽  
The Sun ◽  
Amplitude Scintillation ◽  
Interplanetary Plasma ◽  
The Crab Nebula

Regions of the interplanetary medium currently inaccessible to space vehicles may conveniently be studied using the radio scattering properties of the interplanetary plasma. These effects may give rise to angular broadening of radio sources sufficiently close to the Sun, or to amplitude scintillation of sources of small angular size.

scholarly journals Relationship Between Pulsar and Nebula

1971 ◽  
Vol 46 ◽  
pp. 389-391
Author(s):  
L. Woltjer
Keyword(s):  
Magnetic Field ◽  
Energy Density ◽  
Energy Supply ◽  
Crab Nebula ◽  
Supernova Explosion ◽  
Relativistic Electrons ◽  
The Crab Nebula ◽  
The Magnetic Field

The magnetic field and the relativistic electrons in the Crab Nebula cannot have originated at the time of the supernova explosion. The energy density in the magnetic field is so large that it must have been generated using the energy supply in the pulsar. The energies of the electrons are so high, and their lifetimes correspondingly are so short, that they must have been accelerated, again using the pulsar energy. The efficiency of these processes must be high, but there is an adequate energy supply.

Calibration of the High Energy Replicated Optics to Explore the Sun (HEROES) Hard X-ray Telescope

2014 ◽  
Vol 03 (02) ◽  
pp. 1440007 ◽  
Author(s):  
Colleen A. Wilson-Hodge ◽  
Jessica Gaskin ◽  
Steven Christe ◽  
Albert Shih ◽  
Allyn Tennant ◽  
...  
Keyword(s):  
Crab Nebula ◽  
Grazing Incidence ◽  
High Energy ◽  
Stray Light ◽  
Detector Response ◽  
The Sun ◽  
X Ray ◽  
Laboratory Calibration ◽  
Grazing Incidence Optics ◽  
The Crab Nebula

On 2013 September 21–22, the High Energy Replicated Optics to Explore the Sun (HEROES) hard X-ray telescope flew as a balloon payload from Ft. Sumner, NM. HEROES observed the Sun, the black hole binary GRS 1915+105, and the Crab Nebula during its 27 h flight. In this paper, we describe laboratory calibration measurements of the HEROES detectors using line and continuum sources and applications of these measurements to define channel to energy (gain) corrections for observed events and to define detector response matrices. We characterize the HEROES X-ray grazing incidence optics using measurements taken in the Stray Light Facility (SLF) in Huntsville, AL, and using ray traces. We describe the application of our calibration measurements to in-flight observations of the Crab Nebula.

scholarly journals On the Radio Emitting Particles of the Crab Nebula: Stochastic Acceleration Model

2017 ◽  
Vol 13 (S337) ◽  
pp. 259-262
Author(s):  
Shuta J. Tanaka
Keyword(s):  
Crab Nebula ◽  
Supernova Explosion ◽  
Shock Acceleration ◽  
Back Reaction ◽  
Acceleration Process ◽  
Spectral Evolution ◽  
Stochastic Acceleration ◽  
Acceleration Model ◽  
Pulsar Wind ◽  
The Crab Nebula

AbstractThe standard shock acceleration model of pulsar wind nebulae (PWNe) does not account for the hard spectrum in radio wavelengths. The origin of the radio-emitting particles is also important to determine the pair production efficiency in the pulsar magnetosphere. Here, we propose a possible resolution for the particle energy distribution in PWNe; the radio-emitting particles are not accelerated at the pulsar wind termination shock but are stochastically accelerated by turbulence inside PWNe. We upgrade our past one-zone spectral evolution model including the energy diffusion, i.e., the stochastic acceleration, and apply to the Crab Nebula. For a particle injection to the stochastic acceleration process, we consider the continuous injection from the supernova ejecta or the impulsive injection associated with supernova explosion. The observed broadband spectrum and the decay of the radio flux are reproduced by tuning the amount of the particle injected to the stochastic acceleration process. Our results imply that some unveiled mechanisms, such as back reaction to the turbulence, are required to make the energies of stochastically and shock accelerated particles comparable.

Gold's Fool and God's Country: The Coronado Craze of 1940–1941

Prospects ◽  
1986 ◽  
Vol 11 ◽  
pp. 311-323
Author(s):  
M. Sue Kendall
Keyword(s):  
New Mexico ◽  
Rio Grande Valley ◽  
Rio Grande ◽  
American Southwest ◽  
The Sun ◽  
Far North ◽  
Route Finding

In 1540, a spanish expedition led by Don Francisco Vasquez de Coronado ventured out of Mexico into what is now the American Southwest in search of the Seven Cities of Cibola and the mythical Kingdom of Quivira. The Coronado expedition wandered for two years through present-day Arizona, New Mexico, Texas, and perhaps as far as Oklahoma and Kansas in search of the elusive cities of gold before returning to Mexico, bitter and disappointed. The Spanish conquistadores had set out to find the fabled treasures of Cibola, where, it was rumored, the houses were studded with jewels and the streets were paved with gold. They found instead the source of the inflated legend-the terraced mud pueblos of the Zuñi Indians. The earlier scout, Fray Marcos, had seen them from a distant hillside glittering in the sun, and his vision had been embellished by tales of riches told by the Indians he encountered en route. Finding mud instead of gold, Coronado and his expedition became seduced by tales of yet another land to the east called Quivira, whose riches were beyond imagination and where gold and silver were as common as prairie dust. The quest for the phantom gold of Quivira led Coronado east across the Rio Grande valley and perhaps as far north as present-day Kansas. He had imagined treasures to surpass even those of the Incas in Peru. What he found was another patch of dusty Indian villages, this time made of straw instead of mud. In 1542, the Coronado venture was considered by its Spanish promoters to have been a costly and somewhat embarrassing failure.

Observation of Polarization for the Crab Nebula with PHENEX Polarimeter

2010 ◽  
Vol 8 (ists27) ◽  
pp. Tm_35-Tm_40 ◽  
Author(s):  
Yuji KISHIMOTO ◽  
Shuichi GUNJI ◽  
Yushi ISHIKAWA ◽  
Makoto TAKADA ◽  
Tatehiro MIHARA ◽  
...  
Keyword(s):  
Crab Nebula ◽  
The Crab Nebula

A Model for the Moving “Wisps” in the Crab Nebula

1999 ◽  
Vol 512 (2) ◽  
pp. 755-760 ◽  
Author(s):  
Mitchell C. Begelman
Keyword(s):  
Crab Nebula ◽  
The Crab Nebula

scholarly journals Strong Waves from Pulsars and Morphologies in SNRs

1983 ◽  
Vol 101 ◽  
pp. 499-501
Author(s):  
Gregory Benford ◽  
Attilio Ferrari ◽  
Silvano Massaglia
Keyword(s):  
Large Amplitude ◽  
Crab Nebula ◽  
Surrounding Medium ◽  
Low Frequency ◽  
Optical Emission ◽  
Amplitude Wave ◽  
Surface Magnetic Field ◽  
Plasma Absorption ◽  
The Crab Nebula ◽  
Large Amplitude Wave

Canonical models for pulsars predict the emission of low–frequency waves of large amplitudes, produced by the rotation of a neutron star possessing a strong surface magnetic field. Pacini (1968) proposed this as the basic drain which yields to the pulsar slowing–down rate. The main relevance of the large amplitude wave (LAW) is the energetic link it provides between the pulsar and the surrounding medium. This role has been differently emphasized (Rees and Gunn, 1974; Ferrari, 1974), referring to absorption effects by relativistic particle acceleration and thermal heating, either close to the pulsar magnetosphere or in the nebula. It has been analyzed in the special case of the Crab Nebula, where observations are especially rich (Rees, 1971). As the Crab Nebula displays a cavity around the pulsar of dimension ∼1017cm, the function of the wave in sweeping dense gas away from the circumpulsar region is widely accepted. Absorption probably occurs at the inner edges of the nebula; i.e., where the wave pressure and the nebular pressure come into balance. Ferrari (1974) interpreted the wisps of the Crab Nebula as the region where plasma absorption occurs, damping the large amplitude wave and driving “parametric” plasma turbulence, thus trasferring energy to optical radiation powering the nebula. The mechanism has been extended to interpret the specific features of the “wisps” emission (Benford et al., 1978). Possibly the wave fills the nebula completely, permeating the space outside filaments with electromagnetic energy, continuously accelerating electrons for the extended radio and optical emission (Rees, 1971).

scholarly journals Quantification of Elemental Contaminants in Unregulated Water across Western Navajo Nation

2019 ◽  
Vol 16 (15) ◽  
pp. 2727 ◽  
Author(s):  
Jonathan Credo ◽  
Jaclyn Torkelson ◽  
Tommy Rock ◽  
Jani C. Ingram
Keyword(s):  
Native American ◽  
New Mexico ◽  
Hard Rock ◽  
Water Systems ◽  
American Southwest ◽  
Western United States ◽  
Navajo Nation ◽  
Hard Rock Mining ◽  
Rock Mining ◽  
American Nation

The geologic profile of the western United States lends itself to naturally elevated levels of arsenic and uranium in groundwater and can be exacerbated by mining enterprises. The Navajo Nation, located in the American Southwest, is the largest contiguous Native American Nation and has over a 100-year legacy of hard rock mining. This study has two objectives, quantify the arsenic and uranium concentrations in water systems in the Arizona and Utah side of the Navajo Nation compared to the New Mexico side and to determine if there are other elements of concern. Between 2014 and 2017, 294 water samples were collected across the Arizona and Utah side of the Navajo Nation and analyzed for 21 elements. Of these, 14 elements had at least one instance of a concentration greater than a national regulatory limit, and six of these (V, Ca, As, Mn, Li, and U) had the highest incidence of exceedances and were of concern to various communities on the Navajo Nation. Our findings are similar to other studies conducted in Arizona and on the Navajo Nation and demonstrate that other elements may be a concern for public health beyond arsenic and uranium.

scholarly journals The Crab nebula variability at short time-scales with the Cherenkov telescope array

2020 ◽  
Vol 501 (1) ◽  
pp. 337-346
Author(s):  
E Mestre ◽  
E de Oña Wilhelmi ◽  
D Khangulyan ◽  
R Zanin ◽  
F Acero ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Crab Nebula ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Telescope Array ◽  
Cherenkov Telescopes ◽  
Cherenkov Telescope ◽  
Emission Models ◽  
Short Time ◽  
The Crab Nebula

ABSTRACT Since 2009, several rapid and bright flares have been observed at high energies (>100 MeV) from the direction of the Crab nebula. Several hypotheses have been put forward to explain this phenomenon, but the origin is still unclear. The detection of counterparts at higher energies with the next generation of Cherenkov telescopes will be determinant to constrain the underlying emission mechanisms. We aim at studying the capability of the Cherenkov Telescope Array (CTA) to explore the physics behind the flares, by performing simulations of the Crab nebula spectral energy distribution, both in flaring and steady state, for different parameters related to the physical conditions in the nebula. In particular, we explore the data recorded by Fermi during two particular flares that occurred in 2011 and 2013. The expected GeV and TeV gamma-ray emission is derived using different radiation models. The resulting emission is convoluted with the CTA response and tested for detection, obtaining an exclusion region for the space of parameters that rule the different flare emission models. Our simulations show different scenarios that may be favourable for achieving the detection of the flares in Crab with CTA, in different regimes of energy. In particular, we find that observations with low sub-100 GeV energy threshold telescopes could provide the most model-constraining results.

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