A White Dwarf’s Surprise Planetary Companion

Astronomers have used the international Gemini Observatory, a Program of NSF’s NOIRLab, and other telescopes around the globe and in space to find and characterize a giant planet, less than 13.8 times as massive as Jupiter [1], orbiting a white dwarf star [2][3]. The research is published in the journal Nature.

This is the first example of an intact giant planet orbiting close to a white dwarf star — in this case a particularly cool and dim stellar ember known as WD 1856+534. “The discovery came as something of a surprise,” according to lead author Andrew Vanderburg, assistant professor at the University of Wisconsin-Madison. “A previous example of a similar system, where an object was seen to pass in front of a white dwarf, showed only a debris field from a disintegrating asteroid.” [4]

After detecting the planet with the TESS satellite, which observed it transiting its white dwarf star, the team took advantage of the tremendous light-collecting power of Gemini North’s 8.1-meter mirror and used the sensitive Gemini Near-Infrared Spectrograph (GNIRS) to make detailed measurements of the white dwarf star in infrared light from Maunakea, Hawai‘i. The spectroscopic observations captured the unique fingerprint of the star, but not that of the planet or any debris surrounding this system [5][6]. “Because no debris from the planet was detected floating on the star’s surface or surrounding it in a disk we could infer that the planet is intact,” said Siyi Xu, an assistant astronomer at Gemini Observatory and one of the researchers behind the discovery.

“We were using the TESS satellite to search for transiting debris around white dwarfs, and to try to understand how the process of planetary destruction happens,” explains Vanderburg. “We were not necessarily expecting to find a planet that appeared to be intact.”

“Additionally, because we didn’t detect any light from the planet itself, even in the infrared, it tells us that the planet is extremely cool, among the coolest we’ve ever found.” [7]. Xu adds that the precise upper limit of the planet’s temperature was measured by NASA’s Spitzer Space Telescope to be 17 °C (63 °F), which is similar to the average temperature of Earth. 

“We’ve had indirect evidence that planets exist around white dwarfs and it’s amazing to finally find a planet like this,” said Xu [8]. White dwarfs are extremely dense and very small, so the exoplanet is much larger than its tiny parent star, making the system extremely unusual.

The surprising discovery of this planet, known as WD 1856b, raises interesting questions about the fate of planets orbiting stars destined to become white dwarfs (like our Sun). Of the thousands of planets outside the Solar System that astronomers have discovered, most orbit stars that will eventually evolve into red giants and then into white dwarfs. During this process, any planets in close orbits will be engulfed by the star, a fate that WD 1856b somehow managed to avoid.

“Our discovery suggests that WD 1856b must have originally orbited far away from the star, and then somehow journeyed inwards after the star became a white dwarf,” said Vanderburg. “Now that we know that planets can survive the journey without being broken up by the white dwarf’s gravity, we can look for other, smaller planets.”

“The study of planets in extreme locations is giving us new perspectives on the history and fate of the billions of worlds around other stars,” said Martin Still, NSF Program Director for the international Gemini Observatory partnership. “Gemini’s sensitivity was critical in following up the TESS space-based detection of this planet, revealing a more complete story of the exoplanetary system.”

This new discovery suggests that planets can end up in or near the white dwarf’s habitable zone, and potentially be hospitable to life even after their star has died. “We’re planning future work to study this planet’s atmosphere with Gemini North,” concludes Xu. “The more we can learn about planets like WD 1856b, the more we can find out about the likely fate of our own Solar System in about 5 billion years when the Sun becomes a white dwarf.” [9]

Notes

[1] The upper limit of the object’s mass is 13.8 Jupiter masses. This mass is close to the dividing line astronomers use to distinguish between a planet and a brown dwarf.

[2] White dwarfs are common stellar remnants left behind by the deaths of low-mass stars like the Sun. Though they have a mass comparable to the Sun’s, they are roughly the size of Earth, making them incredibly dense. White dwarfs generate no energy of their own and glow faintly with leftover thermal energy, slowly fading over billions of years.

[3] The discovery of WD 1856b relied on observations from facilities including Gemini North, NASA’s Transiting Exoplanet Survey Satellite (TESS), NASA’s Spitzer Space Telescope, various professional telescopes around the world, and a handful of privately operated telescopes.

[4] Result reported by NASA.

[5] The light from a star is spread over many wavelengths, and not all these wavelengths radiate equally. The distribution of emission at different wavelengths makes up the emission spectrum of a star, and features of this spectrum act as very recognizable “fingerprints.” When an orbiting planet gravitationally tugs at a star, it causes a star to wobble and these spectral fingerprints shift slightly. This technique is often used to gather information about exoplanets, but in the case of WD 1856, the stellar spectrum obtained by Gemini North showed no identifying features — no “fingerprints” — showing that the orbiting planet is intact.

[6] The first “polluted white dwarf” — a white dwarf with planet debris in its outer layer — was discovered in 1917 by Adriaan van Maanen using Mount Wilson observatory’s 60-inch telescope. The star is known as van Maanen’s Star and has an interesting backstory. 

[7] The team was searching at a wavelength of 4.5 microns.

[8] In a result widely reported last year, a team using ESO facilities detected gas disk orbiting, and accreting onto, a white dwarf. The gas seems to have a composition similar to that of Neptune and Uranus, so it is hypothesized that the gas must have come from such a planet. The planet itself was not detected, only the gas debris. 

[9] This could be the final fate of Earth and the other rocky planets in the Solar System. When the Sun expands into a red giant it will swell and become vastly more luminous, charring and then engulfing Mercury, Venus, and possibly Earth. However, there’s nothing to worry about yet — our Sun is only halfway through its 10-billion-year lifetime.

More information 

This research was presented in the paper A Giant Planet Candidate Transiting a White Dwarf to appear in the journal Nature.

The team was composed of Andrew Vanderburg (University of Wisconsin-Madison and University of Texas at Austin), Saul A. Rappaport (Massachusetts Institute of Technology), Siyi Xu (NSF’s NOIRLab/Gemini Observatory), Ian Crossfield (University of Kansas), Juliette C. Becker (California Institute of Technology), Bruce Gary (Hereford Arizona Observatory), Felipe Murgas (Instituto de Astrofísica de Canarias and Universidad de La Laguna), Simon Blouin (Los Alamos National Laboratory), Thomas G. Kaye (Raemor Vista Observatory and The University of Hong Kong), Enric Palle (Instituto de Astrofísica de Canarias and Universidad de La Laguna), Carl Melis (University of California, San Diego), Brett Morris (University of Bern), Laura Kreidberg (Max Planck Institute for Astronomy and Center for Astrophysics | Harvard & Smithsonian), Varoujan Gorjian (NASA Jet Propulsion Laboratory), Caroline V. Morley (University of Texas at Austin), Andrew W. Mann (University of North Carolina at Chapel Hill), Hannu Parviainen (Instituto de Astrofísica de Canarias and Universidad de La Laguna), Logan A. Pearce (University of Arizona), Elisabeth R. Newton (Dartmouth College), Andreia Carrillo (University of Texas at Austin), Ben Zuckerman (University of California, Los Angeles), Lorne Nelson (Bishop’s University), Greg Zeimann (University of Texas at Austin), Warren R. Brown (Center for Astrophysics | Harvard & Smithsonian), René Tronsgaard (Technical University of Denmark), Beth Klein (University of California, Los Angeles), George R. Ricker (Massachusetts Institute of Technology), Roland K. Vanderspek (Massachusetts Institute of Technology), David W. Latham (Center for Astrophysics | Harvard & Smithsonian), Sara Seager (Massachusetts Institute of Technology), Joshua N. Winn (Princeton University), Jon M. Jenkins (NASA Ames Research Center), Fred C. Adams (University of Michigan), Björn Benneke (Université de Montréal), David Berardo (Massachusetts Institute of Technology), Lars A. Buchhave (Technical University of Denmark), Douglas A. Caldwell (NASA Ames Research Center and SETI Institute), Jessie L. Christiansen (Caltech/IPAC-NASA Exoplanet Science Institute), Karen A. Collins (Center for Astrophysics | Harvard & Smithsonian), Knicole D. Colón (NASA Goddard Space Flight Center), Tansu Daylan (Massachusetts Institute of Technology), John Doty (Noqsi Aerospace, Ltd.), Alexandra E. Doyle (University of California, Los Angeles), Diana Dragomir (University of New Mexico, Albuquerque), Courtney Dressing (University of California, Berkeley), Patrick Dufour (Université de Montréal), Akihiko Fukui (Instituto de Astrofísica de Canarias and The University of Tokyo), Ana Glidden (Massachusetts Institute of Technology), Natalia M. Guerrero (Massachusetts Institute of Technology), Xueying Guo (Massachusetts Institute of Technology), Kevin Heng (University of Bern), Andreea I. Henriksen (Technical University of Denmark), Chelsea X. Huang (Massachusetts Institute of Technology), Lisa Kaltenegger (Cornell University), Stephen R. Kane (University of California, Riverside), John A. Lewis (Center for Astrophysics | Harvard & Smithsonian), Jack J. Lissauer (NASA Ames Research Center), Farisa Morales (NASA Jet Propulsion Laboratory and Moorpark College), Norio Narita (National Astronomical Observatory of Japan, Instituto de Astrofísica de Canarias and The University of Tokyo), Joshua Pepper (Lehigh University), Mark E. Rose (NASA Ames Research Center), Jeffrey C. Smith (SETI Institute and NASA Ames Research Center) Keivan G. Stassun (Vanderbilt University and Fisk University), Liang Yu (Massachusetts Institute of Technology and ExxonMobil Upstream Integrated Solutions).

NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab), the US center for ground-based optical-infrared astronomy, operates the international Gemini Observatory (a facility of NSF, NRC–Canada, ANID–Chile, MCTIC–Brazil, MINCyT–Argentina, and KASI–Republic of Korea), Kitt Peak National Observatory (KPNO), Cerro Tololo Inter-American Observatory (CTIO), the Community Science and Data Center (CSDC), and the Vera C. Rubin Observatory. It is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with NSF and is headquartered in Tucson, Arizona. The astronomical community is honored to have the opportunity to conduct astronomical research on Iolkam Du’ag (Kitt Peak) in Arizona, on Maunakea in Hawaiʻi, and on Cerro Tololo and Cerro Pachón in Chile. We recognize and acknowledge the very significant cultural role and reverence that these sites have to the Tohono O’odham Nation, to the Native Hawaiian community, and to the local communities in Chile, respectively.

Links

• Research paper (Nature)
• Companion paper (Astrophysical Journal Letters)
• Photos of the Gemini Telescopes
• NASA video
• NASA release
• IPAC release
• Bishop’s University release
• Vanderbilt University release
• Cornell University release
• University of Texas at Austin release
• University of Wisconsin release
• Heising-Simons Foundation release
• University of Kansas release 
• University of California, Riverside release
• Instituto de Astrofísica de Canarias release
• University of Hong Kong release
• University of Tokyo/Japan Science and Technology Agency release
• Space Scoop

Science Contacts:

Andrew Vanderburg

University of Wisconsin-Madison

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Email [email protected]

Siyi Xu

NSF’s NOIRLab

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