T Pyxidis
{{Short description|Recurrent nova star in the constellation Pyxis}}
{{Starbox begin
| name = T Pyxidis
}}
{{Starbox image
| image = 250px
| caption = T Pyx surrounded by the nova remnants of a previous outburst. Hubble Space Telescope composite
}}
{{Starbox observe
| epoch = J2000
| constell = Pyxis
| dec = {{DEC|−32|22|47.5033}}
| appmag_v = 6.4 Max.
18.5 Min.
}}
{{Starbox character
| class = White Dwarf
| b-v =
| u-b =
| variable = Recurrent nova
}}
{{Starbox astrometry
| radial_v =
| prop_mo_ra = {{val|−2.531|0.052}}
| prop_mo_dec = {{val|0.177|0.062}}
| parallax = 0.3051
| p_error = 0.0419
| dist_pc = {{val|3185|607|283}}
| absmag_v =
}}
{{Starbox detail
| component1 = White dwarf
| mass = {{val|0.7|0.2}}
| component2 = Second component
| mass2 = {{val|0.14|0.03}}
}}
{{Starbox orbit
| period_unitless = 1.8295 hours
| inclination = {{val|10|2}}
}}
{{Starbox catalog
| names = {{odlist | name=Nova Pyx 1890 | name2=AAVSO 0900-31 | 2MASS=J09044150-3222474 | Gaia DR2=5628258258606112768 }}
}}
{{Starbox reference
| Simbad = V*+T+Pyx
}}
{{Starbox end}}
T Pyxidis (T Pyx)According to the Argelander system of nomenclature for variable stars, the initial letter is an R, and the counter progresses alphabetically. Thus, T Pyx is the third variable star in the constellation Pyx. is a recurrent nova{{cite journal|
display-authors=4|
author=Shara, Michael M.|
author2=Zurek, David R.|
author3=Williams, Robert E.|
author4=Prialnik, Dina|
author5=Gilmozzi, Roberto|
author6=Moffat, Anthony F. J. |title=HST Imagery of the Non-Expanding, Clumped "Shell" of the Recurrent Nova T Pyxidis |date=June 1997 |journal=Astronomical Journal |volume=114 | number=1 |pages=258 |bibcode=1997AJ....114..258S |doi = 10.1086/118470 }}
and nova remnant in the constellation Pyxis. It is a binary star system and its distance is estimated at {{convert|4783|pc|ly|abbr=off}} from Earth. It contains a Sun-like star and a white dwarf. Because of their close proximity and the larger mass of the white dwarf, the latter draws matter from the larger, less massive star. The influx of matter on the white dwarf's surface causes periodic thermonuclear explosions to occur.
The usual apparent magnitude of this star system is 15.5, but there have been observed eruptions with maximal apparent magnitude of about 7.0 in the years 1890, 1902, 1920, 1944, 1966 and 2011.{{cite web |url=http://www.aavso.org/aavso-alert-notice-436 |title=Outburst of the recurrent nova T Pyx |date=2011 |publisher=AAVSO }}
Evidence seems to indicate that T Pyxidis may have increased in mass despite the nova eruptions, and is now close to the Chandrasekhar limit when it might explode as a supernova.{{cite news
|date=2010-01-05 |title=T Pyxidis Soon To Be A Type Ia Supernova |publisher=Space Daily |url=http://www.spacedaily.com/reports/T_Pyxidis_Soon_To_Be_A_Type_Ia_Supernova_999.html |access-date=2010-01-05 }} When a white dwarf reaches this limit it will collapse under its own weight and cause a type Ia supernova.
Effect on Earth
Because of its relative proximity, some—in particular, Edward Sion, astronomer & astrophysicist at Villanova University, and his team therefrom—contend that a type 1a supernova could have a significant impact on Earth. The received gamma radiation would equal the total (all spectra) radiation of approximately 1,000 solar flares,{{cite web |date=5 December 2009 |title=Will a Nearby Supernova Endanger Life on Earth? |publisher=TASS, The Amateur Sky Survey |author=Richmond, Michael|url=http://www.tass-survey.org/richmond/answers/snrisks.txt |url-status=dead |archive-url=https://web.archive.org/web/20070306114344/http://www.tass-survey.org/richmond/answers/snrisks.txt |archive-date=6 March 2007 }} but the type Ia supernova would have to be closer than {{convert|1000|pc|ly|abbr=off}} to cause significant damage to the ozone layer, and perhaps closer than 500 parsecs. The X-radiation that reaches Earth in such an event, however, would be less than the X-radiation of a single average solar flare.
However, Sion's calculations were challenged by Alex Filippenko of the University of California at Berkeley who said that Sion had possibly miscalculated the damage that could be caused by a T Pyxidis supernova. He had used data for a far more deadly gamma-ray burst (GRB) occurring 1 kiloparsec from Earth, not a supernova, and T Pyxidis certainly is not expected to produce a GRB. According to another expert, "[a] supernova would have to be 10 times closer [to Earth] to do the damage described."{{cite web |date=6 Jan 2010 |title=Will Earth 'Be Wiped Out' by a Supernova? |publisher=Discovery News |author=O'Neill, Ian |url=http://news.discovery.com/space/will-earth-really-be-wiped-out-by-a-local-supernova.html }} Mankind survived when the radiation from the Crab Nebula supernova, at a distance of about 6,500 light-years, reached Earth in the year 1054. A type Ia supernova at a distance of 3,300 light-years would have an apparent magnitude of around -9.3, about as bright as the brightest Iridium (satellite) flares.A type Ia supernova has an absolute magnitude of -19.3, which is how bright it would appear 10 parsecs away. This star is 3,300 ly (1000 pc) away, or roughly 100 times farther. By the inverse square law, it would thus appear 100^2 or 10,000 times dimmer. Each step of 5 magnitudes defined as a factor of 100 in brightness, so 10,000 times dimmer would be 10 magnitudes dimmer, or -9.3.
Recent data indicates his distance estimate is five times too close. Astronomers used NASA's Hubble Space Telescope to observe the light emitted during its latest outburst in April 2011. The team also used the light echo to refine estimates of the nova's distance from Earth. The new distance is 15,600 light-years (4780 pc) from Earth. Previous estimates were between 6,500 and 16,000 light-years (2000 and 4900 pc).{{cite web |url=http://phys.org/news/2013-06-hubble-d-ejected-material-erupting.html |title=Hubble maps 3-D structure of ejected material around erupting star |date=4 Jun 2013 |publisher=NASA, ESA |author=Crotts, A. |author2=Sokoloski, J. |author3=Uthas, H. |author4=Lawrence, S. |name-list-style=amp }}
It has been reported that T Pyx would "soon" become a supernova. However, when Scientific American contacted Sion, it became apparent that "soon" was meant in astronomical terms: Sion said that "soon" in the press announcement meant "[a]t the accretion rate we derived, the white dwarf in T Pyxidis will reach the Chandrasekhar Limit in ten million years."{{cite web |url=http://www.scientificamerican.com/article.cfm?id=supernova-star-too-close-for-comfor-2010-01 |title=Supernova star too close for comfort |date=5 Jan 2010 |publisher=Scientific American }} By that time it will have moved far enough away from the Solar System to have little effect.
File:T-Pyx-Lightcurve-AAVSO.gif light curve of recurrent nova T Pyx from 1 Jan 1966 to 17 Nov 2010. Up is brighter and down is fainter. Day numbers are Julian days. Different colors reflect different bandpasses.]]
2011 outburst
Mike Linnolt detected T Pyx's first outburst in nearly 45 years on April 14, 2011, at magnitude 13.[http://www.aavso.org/aavso-alert-notice-436 T Pyxidis has been discovered in outburst], 2011, AAVSO According to AAVSO observers, it reached magnitude 7.5 in the visual and V bands by April 27,{{cite web |url=http://www.skyandtelescope.com/community/skyblog/observingblog/119918979.html |title=T Pyxidis Finally Blows Again |publisher=Sky and Telescope |access-date=April 30, 2011 }} and reached magnitude 6.8 by May 3.{{cite web |url=http://www.skyandtelescope.com/community/skyblog/observingblog/119918979.html |title=Sky & Telescope Observing Blog |access-date=May 7, 2011 }}
File:T-Pyx-Lightcurve-2011-Eruption-AAVSO.jpg light curve of recurrent nova T Pyx from April 13 to May 6, 2011. Up is brighter and down is fainter.]]
X-ray source
T Pyxidis is a super soft X-ray source.{{cite journal |display-authors=4 |author=Ogley, R. N. |author2=Chaty, S. |author3=Crocker, M. |author4=Eyres, S. P. S. |author5=Kenworthy, M. A. |author6=Richards, A. M. S. |author7=Rodriguez, L. F. |author8=Stirling, A. M. |title=A search for radio emission from Galactic supersoft X-ray sources |date=Apr 2002 |journal=Monthly Notices of the Royal Astronomical Society |volume=330 |issue=4 |pages=772–7 |doi=10.1046/j.1365-8711.2002.05130.x |doi-access=free |arxiv=astro-ph/0111120 |bibcode=2002MNRAS.330..772O |s2cid=3047485 }}
References
External links
- AAVSO Variable Star Of The Month April, 2002: T Pyxidis [http://chart.aavso.org/sites/default/files/vsots/0402.pdf PDF] / [http://www.aavso.org/vsots_tpyx HTML (17 July 2010)]
- AAVSO: [https://web.archive.org/web/19990824013405/http://ftp.aavso.org/ql/ Quick Look View of AAVSO Observations] (get recent magnitude estimates for T Pyx)
- [https://archive.today/20130415203226/http://www.slackerastronomy.org/wordpress/2009/03/podcast-simo-slacker-interviews-pt-i/ Interview with Brad Schaefer about recurrent novae, and T Pyx] (@19:40 into recording : 30 March 2009)
- [http://astro.corlan.net/stars/PYX/T-PYX.html Variable star T PYXIDIS]
- [http://www.space.com/spacewatch/061222_ns_nova_star.html Astronomers await a nova] (Space.com 22 December 2006)
- Sion, Edward; [http://bigthink.com/ideas/18969 A Supernova Could Nuke Us.] Big Think.
- {{APOD |date=25 September 1997 |title=T Pyxidis: Recurrent Nova}}
- [http://www.space.com/7734-explosive-nearby-star-threaten-earth.html Explosive Nearby Star Could Threaten Earth]
{{Stars of Pyxis}}
{{DEFAULTSORT:T Pyxidis}}