Asset Details
Do you wish to reserve the book?
Fundamental Tests of White Dwarf Cooling Physics with Wide Binaries
Hey, we have placed the reservation for you!
By the way, why not check out events that you can attend while you pick your title.
Oops! Something went wrong.
Looks like we were not able to place the reservation. Kindly try again later.
Are you sure you want to remove the book from the shelf?
Fundamental Tests of White Dwarf Cooling Physics with Wide Binaries
Do you wish to request the book?
Fundamental Tests of White Dwarf Cooling Physics with Wide Binaries
Please be aware that the book you have requested cannot be checked out. If you would like to checkout this book, you can reserve another copy
We have requested the book for you!
Your request is successful and it will be processed during the Library working hours. Please check the status of your request in My Requests.
Oops! Something went wrong.
Looks like we were not able to place your request. Kindly try again later.
Paper
Fundamental Tests of White Dwarf Cooling Physics with Wide Binaries
2024
Overview
We present follow-up spectroscopy and a detailed model atmosphere analysis of 29 wide double white dwarfs, including eight systems with a crystallized C/O core member. We use state-of-the-art evolutionary models to constrain the physical parameters of each star, including the total age. Assuming that the members of wide binaries are coeval, any age difference between the binary members can be used to test the cooling physics for white dwarf stars, including potential delays due to crystallization and \\(^{22}\\)Ne distillation. We use our control sample of 14 wide binaries with non-crystallized members to show that this method works well; the control sample shows an age difference of only \\(\\Delta\\)Age = \\(-0.03 \\pm\\) 0.15 Gyr between its members. For the eight crystallized C/O core systems we find a cooling anomaly of \\(\\Delta\\)Age= 1.13\\(^{+1.20}_{-1.07}\\) Gyr. Even though our results are consistent with a small additional cooling delay (\\(\\sim1\\) Gyr) from \\(^{22}\\)Ne distillation and other neutron-rich impurities, the large uncertainties make this result not statistically significant. Nevertheless, we rule out cooling delays longer than 3.6 Gyr at the 99.7% (\\(3\\sigma\\)) confidence level for 0.6-0.9 \\(M_{\\odot}\\) white dwarfs. Further progress requires larger samples of wide binaries with crystallized massive white dwarf members. We provide a list of subgiant + white dwarf binaries that could be used for this purpose in the future.
Publisher
Cornell University Library, arXiv.org
