Ashley Gonales

Ashley Gonzales
By Ashley Gonzales
Abstract
The genus Helicoprion is preserved by a continuous spiral root that forms the base for more than 130 teeth (Tapanila, L., & Pruitt, J., 2013). This species is found around the world within the Lower Permian marine rocks and at least 100 specimens exist in public collections worldwide (Tapanila, L., & Pruitt, J., 2013). A key characteristic of these species is their teeth whorls. Helicoprion whorls shared a common inner spiral geometry that resulted in large growth of the tooth and root dimensions. These tooth whorls were also the only remains of the fish that were preserved due to its skeletal system being made of cartilage. Being able to cross examine the described tooth whorls of the Helicoprion will allow us to determine its functions and purpose of usage in its environment.
Introduction
The spiral tooth whorl of the Helicoprion has been a spectacle in evolution that has amazed many generations of paleontologists worldwide. This tooth whorl has more than 100 enameloid-covered teeth arranged along a common root that forms a cartilaginous spiral, with the smallest teeth at the axis of the spiral (Tapanila & Pruitt, 2013). The teeth will gradually increase in size away from the spiral center and can exceed 10 centimeters in length (Tapanila & Pruitt, 2013). All Helicoprion teeth have roughly a triangular, laterally compressed, cutting surface that is preserved with serrations with the exception of the juvenile tooth arch that is located at the spiral center (Purdy RW. 2008). The upper crown is then supported by the middle part of the tooth while the lower projections of individual teeth curve in an abaxial direction so that the root of one tooth is shingled below the crown of the other (Purdy RW. 2008). The lower projection of the enameloid does not cover the lowermost part of the root, and this exposed portion is called the shaft (Obruchev DV. 1953). The shaft of the root rests on top of cartilage that encloses the previous evolution of teeth. In a complete whorl, the abaxial part of the spiral ends with an extended root that does not have a middle or upper portion of the tooth crown (Lebedev OA. 2009). Since the Helicoprion whorls are found often preserved at the center of a nodule, this can then pose a couple of obstacles as the cartilaginous jaw and postcranial elements are not preserved within the nodule structure.
Despite this obstacle, Bendix-Almgreen was able to describe the only known Helicoprion specimen, IMNH 37899, also known as ‘Idaho 4’ (Bendix-Almgreen SE. 1966), preserves endoskeletal elements in association with the whorl. The fossil is embedded in a slab of phosphatic limestone from the Early Permian (270 Ma) Phosphoria Formation of Idaho, USA. With limited exposure, Bendix-Almgreen interpreted the calcified layers of cartilage as the jaws and anterior portion. Bandix-Almgreen then created a reconstruction where in his reconstruction, placed the tooth whorl at the front midline of the elongated lower jaws (Bendix-Almgreen SE. 1966, Matsen B& Troll R. 1994), and his interpretation of a neurocranial capsule and rostrum led to his conclusion that the Helicoprion belonged to the Elasmobranchii. Bendix-Almgreen's symphyseal reconstruction (Lebedev OA. 2009, Zangerl R. 1981) has not yet been challenged by new physical evidence until a study conducted in 2013. The phylogenetic interpretations of the Helicoprion and its spiral-tooth relatives have been less vindictive but with most recent analyses and studies based on dental characters, it has placed the Helicoprion among the Euchondrocephali, which include modern chimera and ratfish (Lund R& Grogan ED. 1997, Ginter M, Hampe O& Duffin C. 2010).
Methodology
In a study conducted by a group of scientists at ISU in 2013, they had reexamined the rock slab containing IMNH 37899. IMNH 37899 was scanned using an ACTIS scanner at the University of Texas High-Resolution X-ray CT Facility with a voxel resolution of 0.295 mm in the x- and y-planes, and 1 mm resolution in the z-plane (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). The volume data was reconstructed using the Mimics v. 14.11, Geomagic Studio 2012 and Blender v. 2.64a (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). Since the whorl and teeth of IMNH 37899 are preserved mostly as external impressions, a model of the whorl was created. This computer generated model was produced by scanning and sculpting a three-dimensional whorl using the Blender v. 2.64a software and was used to accurately model the thickness of the teeth and root (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). The model whorl was then scaled to match a surface scan of IMNH 37899, made using a KonicaMinolta Vivid9i non-contact laser scanner at the Idaho Virtualization Lab of IMNH (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
Description
From using these methods the group of scientists were able to give a description of the fossil. IMNH 37899 has been described to have a whorl measuring 23 centimeters in diameter and bearing 117 serrated tooth crowns preserved as impressions (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). The series of tooth crowns are described to be anchored to a continuous osteodentin root and a calcified cartilaginous base that forms a logarithmic spiral of 3¼ revolutions, with the tooth size increasing outward from the spiral center (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). Prismatic calcified cartilage layers of the mandibular arch have lower density than the rock matrix, and are shown in CT scans to be largely intact throughout the specimen (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
Findings
The CT scans conducted reveal that the complete upper left and lower jaws are in a closed articulated position around the medial tooth whorl (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). A large wedge of cartilage is shown to extend from the lower jaw and braces against the outermost root of the whorl (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). The inner parts of the whorl are surrounded by coarse prismatic tessellated cartilage (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
The upper jaw has also been shown to be composed of a triangular palatoquadrate (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). Its posterior border flares laterally for its entire length, and medial to this is a vertical basis trabecular fossa and basal process (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). The quadrate process displays the dual jointed articular surfaces that correspond with the respective articular surfaces of the lower jaw , that is the Meckelian cartilage, which is a primitive feature of jawed vertebrates (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). It was also found that the elongate palatine ramus narrows anteriorly, having a pronounced medial circular dome-shaped ethmoid process (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). In the scans there was no evidence of a groove on the medial surface of the quadrate to accommodate the hyomandibula, and the CT scans provided no evidence for dentition associated with the palatoquadrate (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
The Meckelian cartilage of the lower jaw is described to be incomplete in its posteroventral region. It has been described that its anteroventral surface flares laterally to border the quadratic mandibular fossa ventrally (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). On the Meckelian cartilage anterior to the jaw joint, a “process projects dorsally and abuts a descending process of the palatoquadrate” (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). These processes were hypothesized to serve to restrict closure of the lower jaw, and in turn, prevent the tooth whorl from puncturing the neurocranium (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
In addition, the labial cartilage is a distinctive trait that forms a synchondrosis with the dorsal surface of the Meckelian cartilage making it a unique articulation that is only found in the Helicoprion (Karpinsky AP. 1911). It was also described how the widened portions of the blade-shaped labial cartilage match the dorsal position of successive roots in the whorl, which proposes a gliding articulation with the base of the root (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). In addition, the posterior region of the labial cartilages forms a cup-shaped structure that surrounds the developing root of the last evolution (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
Lastly, part of the tessellated cartilages that surround the inner parts of the whorl were seen to be visible in the scans and do not appear to articulate directly with the lower jaw or the labial cartilages (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). From the surface view of the embedded fossil, these thin cartilage layers are restricted to the ventral and central parts of the whorl (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). It was also shown in the scans that only the outermost eight tooth crowns and a short arc of root appear in the scan (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
Comparison
This study found that the largest amount of anatomical revision is in the upper jaw from previous works. The anterior part was interpreted by Bendix-Almgreen as the neurocranial cavity and rostrum, but the CT scans show evidence for continuity of calcified cartilage through the palatine and quadrate regions of the upper jaw (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). The scans also show that the anterior part of the lower jaw does not include a projection beyond the whorl nor any evidence for a tooth pavement associated with the upper jaw as previously suggested by Bendix-Almgreen (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). This study also identified the labial cartilages concealed by the rock matrix through the use of the CT scans (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
Discussion
The study’s reconstruction suggests that the tooth whorl is a singular, symphyseal structure of the lower jaw that occupies the full length of the mandibular arch (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). This contrasts with previous symphyseal reconstructions (Bendix-Almgreen SE. 1966, Lebedev OA. 2009) that locates the whorl at the anterior end of an elongate jaw that creates a space between the whorl and the jaw joint (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). In the study’s model, the posterior region of the lower jaw is where larger tooth crowns are produced atop a continuous root that is reinforced laterally by the labial cartilage (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). The gliding movement between the root and labial cartilage serve as the connection between the left and right lower jaws. The continual growth of the whorl will then push the tooth–root complex in a curved movement towards the front of the jaw where it will eventually spiral to form the base of the newest root material. This process will then continue to form successive revolutions (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
This retention of teeth in a continuously growing whorl then requires specialized morphologies such as the supporting labial cartilages that maintain rigidity and alignment of the whorl as it closes between the upper jaws (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). With the jaw articulation next to the whorl, closure of the lower jaw rotates the teeth dorsoposteriorly which provides an effective slicing mechanism for the blade-like serrated teeth and forcing food to the back of the oral cavity (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
To adjust to the continuous growth of the logarithmic whorl this required the proportionate anterior and dorsal expansion of the mandibular arch to incorporate the symphyseal structure (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). Based on the largest diameter whorls in the IMNH collections, Helicoprion jaw length and height could exceed 50 centimeters, which would be close to double the size of IMNH 37899 (Bendix-Almgreen SE. 1966, Lebedev OA. 2009). It has also been observed that the premortal tooth wear is rare in the Helicoprion (Bendix-Almgreen SE. 1966, Lebedev OA. 2009). This has been hypothesized to be from the rapid tooth production along with the prey selection of soft-bodied animals, such as cephalopods (Lebedev OA. 2009) or poorly armored fish (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.).
The CT scans in this study revealed that the Helicoprion possessed an autodiastylic jaw suspension (Maisey JG. 2008) distinguished by a two-point articulation of the upper jaw to the neurocranium and the absence of a dorsal extension and hyomandibular articulation site on the upper jaw (Grogan ED& Lund R. 2000). This autodiastylic jaw suspension is diagnostic of euchondrocephalans (Grogan ED, Lund R& Didier D. 1999) which confirms previous dentition-based phylogenies which place the Helicoprion among the Euchondrocephali (Tapanila Leif, Pruitt Jesse, Pradel Alan, Wilga Cheryl D., Ramsay Jason B.,Schlader Robert, Didier Dominique A. 2013.). This result then gives new insight into the evolutionary history of early holocephalans, such as their large body size during the Late Palaeozoic.
Conclusion
In all, these CT scans of the Helicoprion’s tooth whorl gave insight on how it may have looked, worked, and how it may have eaten. It was found that the teeth in the back were “saw-like”, with the jaw creating a rolling back and slicing mechanism. This gave insight that the Helicoprion most likely ate soft-tissue prey such as squid rather than preying on creatures with hard shells. With newer technology, such as CT scans and modeling, the Helicoprion was given further analysis to determine new and revised anatomical findings and has given a better understanding on its evolution.
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Abstract
Subduction zones are home to the most seismically active faults on the planet. The shallow megathrust interface of subduction zones host the largest earthquakes and are the only faults capable of M9+ ruptures. Despite this, our knowledge of subduction zone geometry, which may determine the spatial extent and the size of subduction zone earthquakes, is not fully known. Here we use Slab 2 data from the U.S. Geological Survey to find correlation and characteristics of subducting slab depth versus seismicity activity utilizing Terminal and Python to interpolate the data into models. In being able to model slab depth and seismicity activity, these observations may give insight into the hypothesis that dehydration-derived H2O causes intermediate-depth intraslab earthquakes and other dual mechanisms based on their locations and depths. In doing so, this may give insight on the magnitudes of future earthquakes.
Introduction
Subduction zones account for about 90% of the energy released by historical earthquakes globally. These zones will also account for some of the largest earthquakes and are often events that are both damaging and deadly. Being able to have knowledge of the geometry of subducting slabs is significant to understanding the earthquake and tsunami hazards associated with subduction zones. Though several other global subduction zone geometry databases exist, most are limited in either spatial extent or resolution (U.S.G.S), particularly at shallow depths (<50 km), where the largest, most hazardous subduction zone earthquakes (“megathrust” events) occur and where most tsunamigenic earthquakes are located (U.S.G.S). As tsunamis are very sensitive to the geometry of the fault on which slip occurred, detailed knowledge of the shape of the megathrust is critical for hazard assessment (U.S.G.S). In this study, Slab2, a new model describing the 3D geometries of all seismically active subduction zones worldwide, will be utilized to characterize several locations worldwide (Hayes, G., 2018). These model slabs will be from the near-surface to their deepest expressions in the upper mantle. In all, Slab2 models describe the detailed geometry of more than 24 million square kilometers of subducted slabs overall. In particular this study will focus on intermediate (70-300 km) and deep (300-700 km) earthquakes that occur at pressure (P) and temperature (T) conditions. These are most favorable for brittle failure, making their existence a long-standing problem in solid-Earth geophysics (Hayes, G., 2018). The vast majority of these events occur within the downgoing lithosphere in subduction zones. While hypocentral depth distributions within individual slabs vary, there is a global bimodal depth distribution characterized by a decreasing number of events between 70 and 300 km depths and a distinct increase of seismicity in the lower transition zone between 500 and 700 km depths. In this study, the focus will be on both the increase and decrease in seismicity that occurs between 70 to 700 km depths, specifically, plotting their depths against the earthquake depths of the seismicity that have occurred at the slabs, allowing the characterization of the subduction zones.
Observations/Methods:
The models from Slab2 provide comprehensive geometrical analysis of all known slabs gathered by the U.S. Geological Survey data release. The data was then put into code that was created by this study which is available if requested. The data was set to a 10 year time scale and minimum magnitude of 4.0. The compiled data used from the Slab2 dataset was for 14 regions: Caribbean, Central America, Muertos Trough, Himalayas, Hindu Kush, Philippines, Ryukyu, Alaska, South America. Using Terminal and Python, interpolation was done on the slab depth data onto the seismicity data (Fig. 1.0 and Fig. 2.0). The slab depth data was then indexed to remove any seismicity that was not located on the given slab. Lastly, the seismicity was graphed across the slab depth for each region (Fig.3.0).
Analysis
Compiling our results, we found three distinct groups based on earthquake depth against slab depth: no correlation, low correlation, and high correlation. In the models that displayed no correlation, the distribution of earthquake events were random and appeared unrelated to the area of subduction or few are found at all. In the area of low correlation, there were many earthquake events that are disjointed from the subduction zone but some that are seemingly related. The models that had high correlation, the majority of the earthquake events appeared in the subduction zone where the slab was higher in depth.
Discussion and Conclusion
In seeing the three groups of correlation, this may bring to light more on their characteristics and how different subducting slabs vary from one another and their locations, such as why some may see higher correlation and depth versus others that do not. At some locations, if hydrous minerals are present along normal faults in the trench–outer rise region prior to plate subduction, those hydrous minerals may decompose and expel H2O along the faults as the plate subducts to depth (H. Akira, N. Junichi., 2017). It has been proposed that intraslab earthquakes occur along these preexisting planes of weakness that originated as normal faults prior to subduction (Kirby, 1995). It has also been shown in another study that for outer rise events, features of the geometry of the fault system prior to subduction persist down to c. 450 km depth in the subducted slab (H. Akira, N. Junichi., 2017). This suggests that intraslab events down to this depth are caused by the re- activation of preexisting faults containing hydrous minerals that formed prior to subduction (H. Akira, N. Junichi., 2017). This can also be true for intermediate-depth intraslab events in the Middle America and Chile subduction zones and their models. It is also hypothesized that many of these events occur at the phase boundaries of dehydration reactions across which H2O content changes (H. Akira, N. Junichi., 2017). This study can also hypothesize the existence range of hydrous minerals and the locations of the facies boundaries of dehydration reactions within the slabs beneath the subduction zones of Cascadia, Costa Rica and NE and SW Japan.
In a nature article titled Deep earthquakes in subducting slabs hosted in highly anisotropic rock fabric, it quotes “Yet about 30% of the global earthquakes from the International Seismological Centre (ISC) catalog are deep earthquakes associated with subducting slabs”, which may give reason as to why there were some locations that had no correlation (Li, J., Zheng, Y., Thomsen, L. et al., 2018). Another reason why there may not be or little correlation between the earthquake depth and slab depth is that the fault may be in a “locked” state. For example, in the Cascadia Subduction Zone, it has been the site of “megathrust” earthquakes, but is quiet at present. Stress is likely building up as the Fuca plate continues to subduct beneath North America.
To conclude, it is probable that intermediate-depth intraslab earthquakes occur within the existence range of hydrous minerals in the slab crust and slab mantle. Through distincting differences between the slab depth and seismicity around the world, this will give insight on the state of subducting slabs and how it will affect the surrounding environment. This study could be further investigated through improving the accuracy of the models, adding a temperature model, increasing the spatial resolution of seismic tomography imaging of the internal structures of subducting slabs, and deepening our understanding of the detailed processes that lead to earthquake rupture from a state of local excess pore fluid pressure based on rock deformation experiments or numerical simulations.
Figures
Figure 1.0 (Interpolation figures)







Figure 2.0 (Interpolation)
Figure 3.0 (Slab depth vs. Seismicity)













References
Hayes, G., 2018, Slab2 - A Comprehensive Subduction Zone Geometry Model: U.S. Geological
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H. Akira, N. Junichi., 2017. Seismic imaging of slab metamorphism and
genesis of intermediate-depth intraslab earthquakes. Progress in Earth and Planetary
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Li, J., Zheng, Y., Thomsen, L. et al., 2018. Deep earthquakes in subducting slabs hosted in highly
anisotropic rock fabric. Nature Geosci 11, 696–700.
https://doi.org/10.1038/s41561-018-0188-3
Kirby, Stephen.1995. Interslab earthquakes and phase changes in subducting lithosphere.
Reviews of Geophysics. 33. 287. 10.1029/95RG00353.
Abstract
In definition, binary systems are a system of two astronomical bodies that contain enough gravitational attraction for them to orbit around each other. Within this category, researchers have classified different binary systems into categories, one being a binary pulsar. A binary pulsar system contains a pulsar with a binary companion, often being a white dwarf or a neutron star. In this study we will seek to examine the binary pulsar AR-Sco, specifically the X-ray spectra of the AR Sco Binary System. The spectra of AR-Sco will be achieved through the usage of NuSTAR as it is able to observe a broader range of X-ray energies and penetrate deeper into the region around a binary system, allowing us to observe what emission mechanisms are taking play. The instruments used for the data analysis include the usage of the focusing optics conical Wolter-I telescopes and the Focal Plane Module A of NuSTAR to collect the spectra of AR-Sco, and the following computer programs; Python, Terminal, RFit, XSpec, and Virtual Box. In using these instruments, we aim to determine the best fit models for our observed spectra of AR-Sco to determine the emission mechanism.
Background
AR Sco, is a binary system containing a white dwarf and a main sequence star. The system is composed of a cool, low-mass star in a tight, 3.55-hour orbit with a more massive white dwarf (Marsh et al. 2016). In a study done by Marsh et al. it revealed magnetic interactions between the two component stars, coupled with synchrotron radiation from the white dwarf, power the observed polarized and non-polarized emission (Marsh et al. 2016). AR Sco is therefore the first example of a white dwarf pulsar. In this same study, AR Sco displayed large-amplitude, highly periodic pulsations across the electromagnetic spectrum on a time scale of minutes (Marsh et al. 2016; Takata et al. 2018). Marsh et al., concluded that there appears to be little accretion observed on the white dwarf from its M-dwarf companion (Marsh et al. 2016; Takata et al. 2017), meaning gravitational potential energy is not the source of the emission.
In a study conducted by Stiller et al. in 2018, it was found the minimum of the optical light curve in this study occurs slightly later than zero orbital phase and the optical maximum occurs slightly before phase 0.5 (Stiller et al., 2018). The group of researchers concluded that even after removing the effects of the pulsed radiation from the light curve, the times of minimum and maximum are offset from the orbital alignment (Stiller et al. 2018). The goal of our study is to investigate this offset to further investigate its physical properties to determine the emission mechanism of the compact binary system AR-Sco through its X-ray spectra. We will apply fitting X-ray spectra techniques with XSpec to determine where the emission originates in the system. We will then analyze and discuss the impact of these structures in possible models for the source of energy driving the unusual emission in AR Sco.
Scientific Justification
X-ray spectroscopy from NuSTAR will allow us to answer questions about AR-Sco:
What does AR-Sco’s spectra tell us about the relationship between the white dwarf and the star? Being able to confirm that this is a binary system with a white dwarf and its properties such as mass, will enable us to create a foundation to create models of their relationship.
What does AR-Sco’s spectra tell us about the current state of the binary system? Being able to determine what activity, if any, has been occurring between the two planetary objects will allow us to infer where the emission mechanism is occurring. Doing so, will allow us to determine next steps on what components of the binary system to focus on researching to specify its activity. What can we infer about the future of the AR-Sco binary system based on the spectra? Through determining where the emission mechanism is occurring, this will allow us to create hypotheses on AR-Sco’s future activity and physical state. How does the spectra of AR-Sco change what we expect to observe for future binary systems, specifically those with a white dwarf? Through the discussion of AR-Sco’s spectra, this can not only help us visualize the future of its physical state, but also allow us to evaluate present methods of spectroscopy for all binary systems and our interpretation of binary systems.
Methods and Expected Outcomes:
The instruments that are to be used are the conical Wolter-I telescopes focusing optics at the energy range of 0.3-0.7 keV with an elapsed time of 2 hours. We will use the focal Plane Module A (FPMA) that will allow for precise measurement of the X-ray energies from the energy resolution of 10 keV of NuSTAR. The spectra will be fitted with models in XSpec through the instruments of Python, Terminal, and a Virtual Box. We will use the spectra to determine the flux and the pulsar star’s velocity to determine AR-Sco’s physical properties in order to hypothesize its emission mechanisms. In conducting this study we can expect the fitted X-ray spectra models to not only reveal the physical properties of this binary pulsar, but as well as the emission mechanism, investigating whether the emission arises from a non-thermally heated plasma, which is hypothesized by an earlier study conducted by Singh et al. (Singh et al. 2020).
Spectra Analysis:
In order to analyze the observed data, we will use the methods of fitting the obtained spectra from the NuSTAR detectors. To do so we will utilize Python and XSpec to sort the extracted spectra into bins. Thereafter we will utilize XSpec, Python, and RFit to fit the spectras obtained. Once the models are obtained, we will then select the best fitting models, about two to three, to analyze. Through these spectras we hope to determine not only the several properties of AR-Sco, but also determine the emission mechanism of AR-Sco.
Conclusion:
The exact emission mechanism operating in binary pulsar, AR Sco, continues to be a mystery. In this study we seek to use observations from the NuSTAR X-ray spectroscopy of AR-Sco to delve deeper into AR-Sco’s physical properties and its white dwarf’s relationship to the pulsar. Through the usage of instruments such as XSpec and Python, we can utilize fitting spectra methods to create best fit models of the observed spectra. Our analysis of the modes will enable us to suggest what emission mechanism may be taking place within this binary pulsar.
References:
Marsh, T., Gänsicke, B., Hümmerich, S. et al. A radio-pulsing white dwarf binary star.
Nature 537, 374–377 (2016). https://doi.org/10.1038/nature18620
Singh, K. K., Meintjes, P. J., Kaplan, Q., Ramamonjisoa, F. A., Sahayanathan, S. 2020,
astro-ph.HE, 2006.12950v1.
Singh, K. P., Tandon, S. N., Agrawal, P. C., et al. 2014, Proc. SPIE, Space Telescopes and
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Stiller, R. A., Littlefield, C., Garnavich, P., et al. 2018, AJ,156, 150.
Takata, J., Hu, C.-P., Lin, L.C.C., Tam, P.H.T., Pal, P.S., Hui, C.Y., Kong, A.K.H.,& Cheng, K.S.
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