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Wenjuan Ma

Publications and source records attributed to Wenjuan Ma.

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Using OAI Overlay to Enhance REST API Fuzzing

REST APIs are widely used in industry. Therefore, a lot of research has been focused on how to automatically generate test cases for REST APIs, with few different open-source fuzzers existing in the literature. For a thorough testing, especially in black-box scenarios, just relying on the information provided in the OpenAPI schemas is not enough. Testers typically need to provide extra input data to help steer the fuzzers in the right direction. Dedicated formats specific to each different fuzzer would work, but they would create a vendor lock-in, as well as increasing cognitive load. The OpenAPI Initiative (OAI) standard Overlay might be a solution to this problem. Such standard enables to define transformations on the OpenAPI schemas, where testers can provide input data in Overlay files where such data is provided as ``examples'' entries. In this paper, we have extended the state-of-the-art fuzzer EvoMaster to support Overlay files natively. Experiments are carried out in industry on five APIs from five enterprises from around the world (e.g., Belgium, China, Germany and Türkiye), including two Fortune500 enterprises as well as a 3-man startup. Our industrial results show that Overlay is a viable solution to better enable black-box fuzzing of REST APIs in industry.

cs.SE

Estimating R-Process Yields from Abundances of the Metal-Poor Stars

The chemical abundances of metal-poor stars provide important clues to explore stellar formation history and set significant constraints on models of the r-process. In this work, we find that the abundance patterns of the light and iron group elements of the main r-process stars are very close to those of the weak r-process stars. Based on a detailed abundance comparison, we find that the weak r-process occurs in supernovae with a progenitor mass range of $\sim11-26M_{\odot}$. Using the SN yields given by Heger & Woosley and the abundances of the weak r-process stars, the weak r-process yields are derived. The SNe with a progenitor mass range of $15M_{\odot}<M<26M_{\odot}$ are the main sites of the weak r-process and their contributions are larger than 80%. Using the abundance ratios of the weak r-process and the main r-process in the solar system, the average yields of the main r-process are estimated. The observed correlations of the [neutron-capture/Eu] versus [Eu/Fe] can be explained by mixing of the two r-process abundances in various fractions.

astro-ph.SR