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While old white dwarfs show evidence of dust accretion, white dwarfs older than ~1 billion years or >7000 K with dusty infrared excess were not detected [175] until the discovery of LSPM J0207+3331 in 2018, which has a cooling age of ~3 billion years. The white dwarf shows two dusty components that are being explained with two rings with ...
The white dwarf existed for 10.21 ±0.22 Gyrs, meaning the total age is 10.7 ±0.3 Gyrs. [1] Cold white dwarfs are often strongly affected by collision induced absorption (CIA) of hydrogen. This can lead to faint optical red and infrared brightness. These white dwarfs are also called IR-faint white dwarfs. WD J2147–4035 is however very red (r ...
First white dwarf with a planet WD B1620−26: 2003 PSR B1620-26 b (planet) This planet is a circumbinary planet, which circles both stars in the PSR B1620-26 system [5] [6] First singular white dwarf with a planet WD 1145+017: 2015 WD 1145+017 b: Planet is extremely small and is disintegrating. First white dwarf that is a pulsar: AR Scorpii A ...
The white dwarf is massive and has a mass of 1.00 ± 0.02 M ☉. The cooling age was determined to be 9.5±0.2 Gyrs and the total age is 9.7±0.2 Gyrs. [3] A more recent work found a higher temperature and younger cooling age of about 6.4 Gyrs. [4] The researchers detected sodium, lithium and weak calcium absorption.
As all white dwarfs steadily radiate away their heat over time, this temperature can be used to estimate its age, thought to be around 3 billion years. [29] The progenitor of this white dwarf had an estimated 2.6 solar masses and remained on the main sequence for about 900 million years. This gives the star an overall age of about 4.1 billion ...
ZTF J1901+1458 (nicknamed Z; formally ZTF J190132.9+145808.7; Gaia ID 4506869128279648512 [1]) is a white dwarf, about 135 light years away roughly in the direction of Epsilon Aquilae, discovered by the Zwicky Transient Facility circa 2021.
About 6% of white dwarfs show infrared excess due to a disk around a white dwarf. [66] In the past only a relative small sample of white dwarf disks was known. [67] Due to advances in white dwarf detection (e.g. with Gaia or LAMOST) and improvement of WISE infrared catalogs with unWISE/CatWISE, the number has increased to hundreds of candidates.
Gliese 440, also known as LP 145-141 or LAWD 37, [4] is an isolated white dwarf located 15.1 light-years (4.6 parsecs) from the Solar System in the constellation Musca. [16] It is the fourth closest known white dwarf to the Sun, after Sirius B, Procyon B, and van Maanen's star. [17]