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| {{Short description|1925 Nova seen in the constellation Pictor}} | |||
| '''RR Pictoris''' was a ], which lit up in the constellation ] in ]. RR Pictoris reached a brightness of 1.2 ]. The brightness of RR Pictoris decreased in 150 days by 3 mag. Today RR Pictoris has a brightness of 9 mag. | |||
| {{Starbox begin | | |||
| ⚫ | name=RR Pictoris }} | ||
| {{Starbox image | |||
| | image= | |||
| {{Location mark | |||
| |image=RRPicLocation.png|alt=|width=280 | |||
| }} | |||
| |caption=Location of RR Pictoris (circled in red) | |||
| }} | |||
| {{Starbox observe | | |||
| ==Coordinates== | |||
| epoch=] (]) | | |||
| *]: 06h 35m 36s.25 | |||
| ra={{RA|06|35|36.063}}<ref name=simbad>{{cite simbad|title=RR Pic|access-date=5 December 2020}} </ref>| | |||
| *]: −62° 38' 22".0 | |||
| dec={{DEC|-62|38|22.29}}<ref name=simbad/>| | |||
| appmag_v=1.2<small>Max.</small><br>12.5<small>Min.</small> | | |||
| constell=] }} | |||
| {{Starbox astrometry | |||
| | radial_v = | |||
| | prop_mo_ra = | |||
| | prop_mo_dec = | |||
| | parallax = | |||
| | p_error = | |||
| | dist_ly = {{convert|511|pc|ly|disp=output number only}}{{±|{{convert|8|pc|ly|disp=output number only}}|{{convert|8|pc|ly|disp=output number only}}}} | |||
| | dist_pc = {{val|511|8|8}} | |||
| <ref name="brad">{{cite journal |last1=Schaefer |first1=Bradley E. |title=The distances to Novae as seen by Gaia |journal=Monthly Notices of the Royal Astronomical Society |date=20 September 2018 |volume=481 |issue=3 |pages=3033–3051 |doi=10.1093/mnras/sty2388 |doi-access=free |arxiv=1809.00180 |bibcode=2018MNRAS.481.3033S }}</ref> | |||
| }} | |||
| {{Starbox character | |||
| | variable = ] | |||
| }} | |||
| {{Starbox catalog | |||
| | names={{odlist|HIP= 31481|TYC=8899-1342-1|V=RR Pic}}, Nova Pic 1925, AAVSO 0634-62, Gaia DR2 5477422099543150592 | |||
| }} | |||
| {{Starbox reference | |||
| | Simbad=RR+Pic | |||
| }} | |||
| {{Starbox end}} | |||
| ] of RR Pictoris from ] data.]] | |||
| ] | |||
| '''RR Pictoris''', also known as '''Nova Pictoris 1925''', is a ] star system that flared up as a ] that lit up in the constellation ] in 1925. It was discovered by South African amateur astronomer R. Watson who lived in ]. At 05:50 AM on 25 May 1925, Mr. Watson was walking to work and noticed a star that he did not recognize in line with the stars ] and ]. He consulted his copy of ], and realized that the unfamiliar star was a nova. Fortuitously, Mr. Watson was employed as a telegraph operator, and he promptly sent a telegram describing his discovery to the Royal Observatory at Cape Town. This quick reporting of the event allowed southern observatories to obtain ] of the nova before it had reached maximum brightness.<ref>{{cite journal |last1=Vandenbos |first1=W.H. |title=Nova Pictoris 1925 |journal=Monthly Notes of the Astronomical Society of South Africa |date=1947 |volume=6 |pages=2–4 |bibcode=1947MNSSA...6....2V |url=http://adsabs.harvard.edu/full/1947MNSSA...6....2V |access-date=5 December 2020}}</ref><ref>{{cite journal |last1=Barritt |first1=Leon |title=Nova Pictoris, 1925 |journal=The Monthly Evening Sky Map |date=February 1926 |volume=XXI |page=1}}</ref> | |||
| At the time of its discovery, RR Pictoris had an ] of 2.3. It continued to brighten to magnitude 1.2, which it reached on 9 June 1925. It dimmed to magnitude 4 by 4 July, but brightened again to 1.9 on 9 August. Six months after its peak brightness, RR Pictoris faded to be invisible to the unaided eye, and was magnitude 12.5 by 1975.<ref name="burnham">{{cite book|last=Burnham|first=Robert |title=Burnham's Celestial Handbook, Volume Three: An Observer's Guide to the Universe Beyond the Solar System|publisher=Courier Dover Publications|location=New York, New York|date=2013|orig-year=1977 |pages=1460–62|isbn=978-0-486-31803-5|url=https://books.google.com/books?id=3drCAgAAQBAJ&pg=PA1460}}</ref><!-- cites para --> RR Pictoris is classified as a slow nova<ref>{{cite web |title=RR Pictoris |url=https://www.aavso.org/lcotw/rr-pictoris |website=aavso.org |publisher=American Association of Variable Star Observers |access-date=5 December 2020}}</ref> and its light curve exhibits positive ]s, meaning superhumps with a period a few percent (8.6% in this case) longer than the star system's orbital period.<ref>{{cite journal |last1=Fuentes-Morales |first1=I. |last2=Vogt |first2=N. |last3=Tappert |first3=C. |last4=Schmidtobreick |first4=L. |last5=Hambsch |first5=F.J. |last6=Vuckovic |first6=M. |title=Photometric long-term variations and superhump occurrence in the Classical Nova RR Pictoris |journal=Monthly Notices of the Royal Astronomical Society |date=February 2018 |volume=474 |issue=2 |pages=2493–2501 |doi=10.1093/mnras/stx2838 |arxiv=1710.06543 |doi-access=free }}</ref> | |||
| Measurements by the ] show that the RR Pictoris system is around 510 parsecs (1670 light-years) from the Earth.<ref name="brad"/> | |||
| Novae are close binary systems composed of a ] and secondary star that is so close it is filling up its ] with stellar material, which is then transferred onto the first star's ]. Once this material reaches a critical mass, it ignites and the system brightens tremendously. The two stars of RR Pictoris orbit each other every 3.48 hours. Calculations of the speed suggest the secondary star is not dense enough for its size to still be on the ], so it itself must have begun expanding and cooling already as its core has run out of hydrogen fuel.<ref name="Ribeiro06">{{cite journal|author=Ribeiro, Fabíola M. A.|author2=Diaz, Marcos P.|date=2006|title=A Tomographic Study of the Classical Nova RR Pictoris|journal=Publications of the Astronomical Society of the Pacific|volume=118|issue=839|pages=84–93|jstor=498458|arxiv = astro-ph/0510042 |bibcode = 2006PASP..118...84R |doi = 10.1086/498458 |s2cid=18244357}}</ref> | |||
| Small variations in the observed orbital period suggest that RR Pictoris system may include a low mass (0.25 ]) third star orbiting the close binary pair with a period of about 70 years.<ref>{{cite journal |last1=Vogt |first1=N. |last2=Schreiber |first2=M.R. |last3=Hambsch |first3=F.J. |last4=Retamales |first4=G. |last5=Tappert |first5=C. |last6=Schmidtobreick |first6=L. |last7=Fuentes-Morales |first7=I. |title=The Orbital Ephemeris of the Classical Nova RR Pictoris: Presence of a Third Body? |journal=Publications of the Astronomical Society of the Pacific |date=January 2017 |volume=129 |issue=971 |page=014201 |doi=10.1088/1538-3873/129/971/014201 |arxiv=1609.05274 |bibcode=2017PASP..129a4201V |s2cid=119183582 }}</ref> | |||
| A small (< 30 arc second) filamentary nebula surrounds the nova, and comparisons of images taken several years apart have allowed its rate of expansion to be measured.<ref>{{cite journal |last1=Williams |first1=R.E. |last2=Gallagher |first2=J.S. |title=Spectrophotometry of filaments surrounding nova RR Pictoris 1925. |journal=The Astrophysical Journal |date=March 1979 |volume=228 |pages=482–490 |doi=10.1086/156869 |bibcode=1979ApJ...228..482W |url=http://articles.adsabs.harvard.edu/pdf/1979ApJ...228..482W |access-date=5 December 2020|doi-access=free }}</ref><ref>{{cite journal |last1=Duerbeck |first1=H.W. |title=The large intractable nova shells |journal=The Messenger |date=December 1987 |volume=80 |pages=8–11 |doi=10.1086/156869 |bibcode=1979ApJ...228..482W |url=http://articles.adsabs.harvard.edu/pdf/1987Msngr..50....8D |access-date=5 December 2020|doi-access=free }}</ref> | |||
| ==References== | |||
| {{reflist}} | |||
| ==External links== | ==External links== | ||
| *{{Dead link|date=September 2023 |bot=InternetArchiveBot |fix-attempted=yes }} | |||
| * http://www.tsm.toyama.toyama.jp/curators/aroom/var/nova/1920.htm | |||
| {{ |
{{Stars of Pictor}} | ||
| ⚫ | {{DEFAULTSORT:RR Pictoris}} | ||
| ] | ] | ||
| ] | ] | ||
| ] | |||
| ] | ] | ||
| ] | |||
| ⚫ | |||
| ] | ] | ||
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Latest revision as of 06:43, 7 October 2024
1925 Nova seen in the constellation Pictor
Location of RR Pictoris (circled in red) | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Pictor |
| Right ascension | 06 35 36.063 |
| Declination | −62° 38′ 22.29″ |
| Apparent magnitude (V) | 1.2Max. 12.5Min. |
| Astrometry | |
| Distance | 1,670 −26 ly (511+8 −8 pc) |
| Characteristics | |
| Variable type | Classical Nova |
| Other designations | |
| RR Pic, HIP 31481, TYC 8899-1342-1, Nova Pic 1925, AAVSO 0634-62, Gaia DR2 5477422099543150592 | |
| Database references | |
| SIMBAD | data |
RR Pictoris, also known as Nova Pictoris 1925, is a cataclysmic variable star system that flared up as a nova that lit up in the constellation Pictor in 1925. It was discovered by South African amateur astronomer R. Watson who lived in Beaufort West. At 05:50 AM on 25 May 1925, Mr. Watson was walking to work and noticed a star that he did not recognize in line with the stars α Crucis and β Carinae. He consulted his copy of Norton's Star Atlas, and realized that the unfamiliar star was a nova. Fortuitously, Mr. Watson was employed as a telegraph operator, and he promptly sent a telegram describing his discovery to the Royal Observatory at Cape Town. This quick reporting of the event allowed southern observatories to obtain spectra of the nova before it had reached maximum brightness.
At the time of its discovery, RR Pictoris had an apparent magnitude of 2.3. It continued to brighten to magnitude 1.2, which it reached on 9 June 1925. It dimmed to magnitude 4 by 4 July, but brightened again to 1.9 on 9 August. Six months after its peak brightness, RR Pictoris faded to be invisible to the unaided eye, and was magnitude 12.5 by 1975. RR Pictoris is classified as a slow nova and its light curve exhibits positive superhumps, meaning superhumps with a period a few percent (8.6% in this case) longer than the star system's orbital period.
Measurements by the Gaia spacecraft show that the RR Pictoris system is around 510 parsecs (1670 light-years) from the Earth.
Novae are close binary systems composed of a white dwarf and secondary star that is so close it is filling up its Roche lobe with stellar material, which is then transferred onto the first star's accretion disc. Once this material reaches a critical mass, it ignites and the system brightens tremendously. The two stars of RR Pictoris orbit each other every 3.48 hours. Calculations of the speed suggest the secondary star is not dense enough for its size to still be on the main sequence, so it itself must have begun expanding and cooling already as its core has run out of hydrogen fuel.
Small variations in the observed orbital period suggest that RR Pictoris system may include a low mass (0.25 M⊙) third star orbiting the close binary pair with a period of about 70 years.
A small (< 30 arc second) filamentary nebula surrounds the nova, and comparisons of images taken several years apart have allowed its rate of expansion to be measured.
References
- ^ "RR Pic". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 5 December 2020.
- ^ Schaefer, Bradley E. (20 September 2018). "The distances to Novae as seen by Gaia". Monthly Notices of the Royal Astronomical Society. 481 (3): 3033–3051. arXiv:1809.00180. Bibcode:2018MNRAS.481.3033S. doi:10.1093/mnras/sty2388.
- Vandenbos, W.H. (1947). "Nova Pictoris 1925". Monthly Notes of the Astronomical Society of South Africa. 6: 2–4. Bibcode:1947MNSSA...6....2V. Retrieved 5 December 2020.
- Barritt, Leon (February 1926). "Nova Pictoris, 1925". The Monthly Evening Sky Map. XXI: 1.
- Burnham, Robert (2013) . Burnham's Celestial Handbook, Volume Three: An Observer's Guide to the Universe Beyond the Solar System. New York, New York: Courier Dover Publications. pp. 1460–62. ISBN 978-0-486-31803-5.
- "RR Pictoris". aavso.org. American Association of Variable Star Observers. Retrieved 5 December 2020.
- Fuentes-Morales, I.; Vogt, N.; Tappert, C.; Schmidtobreick, L.; Hambsch, F.J.; Vuckovic, M. (February 2018). "Photometric long-term variations and superhump occurrence in the Classical Nova RR Pictoris". Monthly Notices of the Royal Astronomical Society. 474 (2): 2493–2501. arXiv:1710.06543. doi:10.1093/mnras/stx2838.
- Ribeiro, Fabíola M. A.; Diaz, Marcos P. (2006). "A Tomographic Study of the Classical Nova RR Pictoris". Publications of the Astronomical Society of the Pacific. 118 (839): 84–93. arXiv:astro-ph/0510042. Bibcode:2006PASP..118...84R. doi:10.1086/498458. JSTOR 498458. S2CID 18244357.
- Vogt, N.; Schreiber, M.R.; Hambsch, F.J.; Retamales, G.; Tappert, C.; Schmidtobreick, L.; Fuentes-Morales, I. (January 2017). "The Orbital Ephemeris of the Classical Nova RR Pictoris: Presence of a Third Body?". Publications of the Astronomical Society of the Pacific. 129 (971): 014201. arXiv:1609.05274. Bibcode:2017PASP..129a4201V. doi:10.1088/1538-3873/129/971/014201. S2CID 119183582.
- Williams, R.E.; Gallagher, J.S. (March 1979). "Spectrophotometry of filaments surrounding nova RR Pictoris 1925". The Astrophysical Journal. 228: 482–490. Bibcode:1979ApJ...228..482W. doi:10.1086/156869. Retrieved 5 December 2020.
- Duerbeck, H.W. (December 1987). "The large intractable nova shells". The Messenger. 80: 8–11. Bibcode:1979ApJ...228..482W. doi:10.1086/156869. Retrieved 5 December 2020.
External links
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