8 research outputs found
An Outbursting Protostar: The environment of L1251 VLA 6
Young protostars that undergo episodic accretion can provide insight into the
impact on their circumstellar environments while matter is accreted from the
disk onto the protostar. IRAS 22343+7501 is a four component protostar system
with one of those being a fading outbursting protostar referred to as L1251 VLA
6. Given the rarity of YSOs undergoing this type of accretion, L1251 VLA 6 can
elucidate the fading phase of the post-outburst process. Here we examine
structure in the disk around L1251 VLA 6 at frequencies of 10 GHz and 33 GHz
with the Karl G. Jansky Very Large Array (VLA). We model the disk structure
using Markov chain Monte Carlo (MCMC). This method is then combined with a
parametric ray-tracing code to generate synthetic model images of an
axisymmetric disk, allowing us to characterize the radial distribution of dust
in the system. The results of our MCMC fit show that the most probable values
for the mass and radius are consistent with values typical of Class I objects.
We find that the total mass of the disk is 0.070^{+0.031}_{-0.2} \rm ~
M_{\sun} and investigate the conditions that could cause the accretion
outburst. We conclude that the eruption is not caused by gravitational
instability and consider alternative explanations and trigger mechanisms.Comment: 16 pages, 9 figures, 5 tables, Accepted in Ap
Connecting Mission Profiles and Radiation Vulnerability Assessment
Radiation vulnerability assessment early in spacecraft development is cheaper and faster than in late development phases. RGENTIC and SEAM are two software platforms that can be coupled to provide this type of early assessment. Specifically, RGENTIC is a tool that outputs descriptions of radiation risks based on a selected mission environment and the system’s electronic part portfolio, while SEAM models how radiation-induced faults in electronic parts propagate through a system. In this work, we propose a spacecraft evaluation flow where RGENTIC’s outputs, which are radiation vulnerabilities of electronic parts for a given mission, become inputs to SEAM, resulting in an automatic part-type template palette presented to users so that they can easily begin modeling the occurrence and propagation of radiation-induced faults in their spacecraft. In this context, fault propagation modeling shows how radiation effects impact the spacecraft’s electronics.
The interface between these platforms can be streamlined through the creation of a SEAM global part-type library with templates based on radiation effects in part-type families such as sensors, processors, voltage regulators, and so forth. Several of the part-types defined in RGENTIC have been integrated into SEAM templates. Ultimately, all 66+ part-types from the RGENTIC look-up table will be included in the SEAM global part library. Once accomplished, the part templates can be used to populate each project-specific part library in SEAM, ensuring all RGENTIC’s part-types are represented, and the radiation effects are consistent between the two.
The harmonization process between RGENTIC and SEAM begins as follows: designers input a detailed knowledge of their system and mission into RGENTIC, which then outputs a generic part-type list that associates each part-type with potential radiation concerns. The list is then downloaded in a SEAM-readable file, which SEAM uses to populate the initially blank project with the part templates that correspond to RGENTIC’s output. The final product is a system fault model using a project-specific radiation effect part library.
The radiation effects considered in the part library are associated with three categories of radiation-environment issues: single event effects (SEE), total ionizing dose (TID), and displacement damage dose (DDD). An example part-type is the discrete LED, which has been functionally decomposed into input power and output light. It has a single possible radiation-induced fault that is associated with DDD, which causes degraded brightness and is observed on the output.
Overall, designers will benefit from a coordination of these two tools because it simplifies the initial definition of the project in SEAM. This is especially the case for new users, since the necessary radiation models for their parts are available before modeling commences. Furthermore, starting from a duplicate of an existing project decreases the amount of time and effort required to develop project-specific models. Incorporating RGENTIC’s table of part-types resolves these issues and provides a streamlined process for creating system radiation fault models. Consequently, spacecraft designers can identify radiation problems early in the design cycle and fix them with lower cost and less effort than in later design stages
Methodology for Correlating Historical Degradation Data to Radiation-Induced Degradation System Effects in Small Satellites
When constructing a system-level fault tree to demonstrate device-to-system level radiation degradation, reliability engineers need relevant, device-level failure probabilities to incorporate into reliability models. Deriving probabilities from testing can be expensive and time-consuming, especially if the system is complex. This methodology offers an alternative means of deriving device-level failure probabilities. It uses Bayesian analysis to establish links between historical radiation datasets and failure probabilities. A demonstration system for this methodology is provided, which is a TID response of a linear voltage regulator at 100 krad(SiO2). Data fed into the Bayesian model is derived from literature on the components found within a linear voltage regulator. An example is presented with data pertaining to the device’s bipolar junction transistor (BJT)’s gain degradation factor (GDF). Kernel density estimation is used to provide insight into the dataset’s general distribution shape. This guides the engineer into picking the appropriate distribution for device-level Bayesian analysis. Failure probabilities generated from the Bayesian analysis are incorporated into a LTspice model to derive a system failure probability (using Monte Carlo) of the regulator’s output. In our demonstration system, a 96.5% likelihood of system degradation was found in the assumed environment
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Resolving Structure in the Debris Disk around HD 206893 with ALMA
Debris disks are tenuous, dusty belts surrounding main-sequence stars generated by collisions between planetesimals. HD 206893 is one of only two stars known to host a directly imaged brown dwarf orbiting interior to its debris ring, in this case at a projected separation of 10.4 au. Here we resolve structure in the debris disk around HD 206893 at an angular resolution of 0.″6 (24 au) and wavelength of 1.3 mm with the Atacama Large Millimeter/submillimeter Array (ALMA). We observe a broad disk extending from a radius of <51 au to 194-2+13 au. We model the disk with a continuous, gapped, and double power-law model of the surface density profile and find strong evidence for a local minimum in the surface density distribution near a radius of 70 au, consistent with a gap in the disk with an inner radius of 63-16+8 au and width 31-7+11 au. Gapped structure has been observed in four other debris disks - essentially every other radially resolved debris disk observed with sufficient angular resolution and sensitivity with ALMA - and could be suggestive of the presence of an additional planetary-mass companion. © 2021. The American Astronomical Society. All rights reserved.Immediate accessThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]
An Outbursting Protostar: The Environment of L1251 VLA 6
Young protostars that undergo episodic accretion can provide insight into the impact on their circumstellar environments while matter is accreted from the disk onto the protostar. IRAS 22343+7501 is a four-component protostar system with one of those being a fading outbursting protostar, which was obseved with the Karl G. Jansky Very Large Array (VLA) and is referred to as L1251 VLA 6. Given the rarity of young stellar objects undergoing this type of accretion, L1251 VLA 6 can elucidate the fading phase of the post-outburst process. Here, we examine structure in the disk around L1251 VLA 6 at frequencies of 10 and 33 GHz with the VLA. We model the disk structure using Markov Chain Monte Carlo (MCMC). This method is then combined with a parametric ray-tracing code to generate synthetic model images of an axisymmetric disk, allowing us to characterize the radial distribution of dust in the system. The results of our MCMC fit show that the most probable values for the mass and radius are consistent with values typical of Class I objects. We find that the total mass of the disk is and investigate the conditions that could cause the accretion outburst. We conclude that the eruption is not caused by gravitational instability and consider alternative explanations and trigger mechanisms