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2. Symbiotic binary - Wikipedia

   en.wikipedia.org/wiki/Symbiotic_binary

   They usually contain a white dwarf with a companion red giant. The cool giant star loses material via Roche lobe overflow or through its stellar wind, which flows onto the hot compact star, usually via an accretion disk. Symbiotic binaries are of particular interest to astronomers as they can be used to learn about stellar evolution.

3. WD J2147–4035 - Wikipedia

   en.wikipedia.org/wiki/WD_J2147–4035

   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 ...

4. White dwarf - Wikipedia

   en.wikipedia.org/wiki/White_dwarf

   The red dwarf spirals inwards towards the core and might merge with the core. If this does not happen and instead the common envelope is ejected, then the binary ends up in a close orbit, consisting of a white dwarf and a red dwarf. This type of binary is called a post-common envelope binary.

5. Subdwarf - Wikipedia

   en.wikipedia.org/wiki/Subdwarf

   It has a mass of 84 to 87 M J, making VVV 1256−62B likely a red dwarf star. [14] The subdwarf Wolf 1130C (sdT8) is the companion of an old subdwarf-white dwarf binary, which is estimated to be older than 10 billion years. It has a mass of 44.9 M J, making it a brown dwarf.

6. G 29-38 - Wikipedia

   en.wikipedia.org/wiki/G_29-38

   Giclas 29-38, also known as ZZ Piscium, is a variable white dwarf star of the DAV (or ZZ Ceti) type, whose variability is due to large-amplitude, non-radial pulsations known as gravity waves. It was first reported to be variable by Shulov and Kopatskaya in 1974.

7. van Maanen 2 - Wikipedia

   en.wikipedia.org/wiki/Van_Maanen_2

   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 years. When this star left the main sequence, it expanded into a red giant that reached a maximum radius of 1,000 times the current radius of the Sun, or ...