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| T Pyxidis | |
|---|---|
| Name | T Pyxidis |
| Epoch | J2000 |
| Constellation | Pyxis |
| Ra | 09h 04m 41.5s |
| Dec | −32° 22′ 47″ |
| Apparent magnitude | 15.5 (quiescence) |
| Spectral type | cataclysmic variable |
| Type | recurrent nova |
| Distance | ~4,800 ly |
T Pyxidis is a recurrent nova in the constellation Pyxis that undergoes semi-regular thermonuclear eruptions on a white dwarf primary in a close binary system. The object has been central to studies of cataclysmic variables, novae, and the progenitor channels of Type Ia supernovae owing to its unusual recurrence interval, complex circumbinary nebula, and implications for mass accumulation. Observations from professional observatories and amateur networks have combined with theoretical work by institutions such as the Harvard College Observatory, Space Telescope Science Institute, and European Southern Observatory to constrain its properties.
T Pyxidis was identified as a recurrent nova with multiple historic eruptions and stands out among systems cataloged by groups like the Royal Astronomical Society and surveys led by the American Association of Variable Star Observers and the All-Sky Automated Survey for Supernovae. Its study intersects research themes pursued at facilities including the Hubble Space Telescope, the Chandra X-ray Observatory, and ground-based sites such as the Very Large Telescope and Keck Observatory, linking it to broader investigations into binary evolution overseen at universities like Harvard University, University of Cambridge, and University of California, Berkeley.
The system was first recorded during early nova searches by observers associated with the Royal Observatory, Cape of Good Hope and later followed through photographic and visual monitoring networks connected to the Harvard Plate Collection and the AAVSO. Key eruptions were recorded in the 20th century by observers from institutions including Mount Wilson Observatory and Palomar Observatory, while modern eruptions prompted rapid response observations by teams at the European Southern Observatory, the National Optical-Infrared Astronomy Research Laboratory, and space missions such as the Hubble Space Telescope and the Swift Observatory. Historical light curve reconstructions have used archival material from the Sonneberg Observatory and plate digitization projects led by the Harvard-Smithsonian Center for Astrophysics.
T Pyxidis is a close interacting binary composed of a degenerate white dwarf primary and a low-mass donor star in a short orbital period system studied by research groups at the Max Planck Institute for Astrophysics and the Institute of Astronomy, Cambridge. Radial velocity and photometric studies by teams at ESO and the Keck Observatory yield an orbital period of order hours, a white dwarf mass estimated from modeling by researchers at MIT and Princeton University, and a donor consistent with a late-type star characterized in surveys like the Two Micron All Sky Survey and the Gaia mission. Spectroscopic analyses employing instrumentation from Gemini Observatory and the Subaru Telescope have identified emission-line profiles and accretion signatures used by modelers at the University of Chicago and the University of Toronto to infer inclination, mass ratio, and accretion rate.
Observed eruptions recorded in archives maintained by the AAVSO, analyzed by researchers at Utrecht University and University of Oxford, exhibit rapid rises and declines in optical bands monitored with telescopes such as the Liverpool Telescope and the Las Cumbres Observatory Global Telescope Network. Multiwavelength campaigns coordinated with teams at the Chandra X-ray Center, European Space Agency, and the National Radio Astronomy Observatory have traced ultraviolet, optical, X-ray, and radio evolution, informing thermonuclear runaway models developed at institutions including Los Alamos National Laboratory and Lawrence Livermore National Laboratory. Comparative studies referencing classical novae recorded by the International Astronomical Union and recurrent systems like those in catalogs from the Smithsonian Astrophysical Observatory place the eruptions in context of accretion-driven ignition cycles studied by theorists at Caltech and University of Arizona.
High-resolution imaging with the Hubble Space Telescope and adaptive optics from the European Southern Observatory revealed a complex, clumpy nebular shell and expanding knots that link to circumbinary material surveyed by the Atacama Large Millimeter/submillimeter Array and the Very Large Array. Studies led by teams at the Space Telescope Science Institute, Smithsonian Astrophysical Observatory, and University of Edinburgh interpreted the morphology as shaped by repeated eruptions and possible pre-existing common-envelope or wind-driven structures, resonating with hydrodynamic simulations performed at the Princeton Plasma Physics Laboratory and the Max Planck Institute for Astrophysics.
Accretion physics in the system has been probed through spectroscopy, time-series photometry, and X-ray monitoring by investigators at MIT, Harvard-Smithsonian Center for Astrophysics, and ESA, revealing high mass-transfer rates potentially driven by irradiation of the donor and angular-momentum loss processes studied at the Institute of Astronomy, Cambridge and University of Southampton. The critical issue of whether the white dwarf gains or loses mass over repeated cycles has been addressed with models from the University of Chicago, Los Alamos National Laboratory, and University of California, Santa Cruz, incorporating results from nucleosynthesis calculations by teams tied to the Joint Institute for Nuclear Astrophysics.
T Pyxidis figures in debates about single-degenerate progenitor channels for Type Ia supernovae examined by collaborations involving the Supernova Cosmology Project, the Sloan Digital Sky Survey, and researchers at University College London and UC Berkeley. Long-term monitoring by the AAVSO, follow-up by space observatories like Chandra and HST, and theoretical predictions from groups at Caltech and the Max Planck Institute for Astrophysics aim to determine whether continued accretion could drive the white dwarf toward the Chandrasekhar limit or whether mass loss prevents supernova detonation, a question that links to cosmology research pursued by the Dark Energy Survey and the European Southern Observatory.
Category:Recurrent novae