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	Perseus (constellation) - Wikipedia, the free encyclopedia
		The stars alpha Persei, gamma Persei, tau Persei, and iota Persei form Perseus' head: gamma Persei is of the third magnitude.
		The stars alpha Persei, psi Persei, delta Persei, 48 Persei, mu Persei, and lambda Persei form Perseus' left arm and hand: delta Persei being of the third magnitude.
		Stars epsilon Persei, xi Persei, zeta Persei, and omicron Persei form Perseus' left leg and foot: zeta Persei being of the third magnitude.
	en.wikipedia.org /wiki/Perseus_(constellation) (920 words)

	GK Per
		The unusual nova shell GK Per is the result of Nova Persei 1901, a nova which exploded in 1901 about 1500 light years away in the direction of the constellation Perseus.
		The first bright nova of the 20th century and the first to be subjected to detailed spectroscopy and photometry, Nova Persei 1901 reached a maximum brightness of 0.2m and declined very rapidly thereafter to its current minimum of 13.1.
		GK Per is unique among classical novae, having the longest known period (almost two days) and showing dwarf nova-like outbursts of about 3 mag.
	www.noao.edu /wiyn/images/gkper.html (420 words)

	Cataclysmic Variables (Site not responding. Last check: 2007-10-24)
		The cataclysmic variable GK Persei, a classical nova system, is one of the more unusual examples of its type: it has the longest known orbital period for a CV (approximately 2 days), and it contains a white dwarf with an evolved K2 sub-giant secondary.
		The 60 and 100 micron emission, as observed by IRAS, is extended to approximately 17 arcminutes to the NW and SE of GK Persei, with the centre of this emission located at the CV.
		Thus, we have demonstrated that GK Persei is a unique laboratory for studies of binary evolution leading to the formation of CV's.
	www.drao-ofr.hia-iha.nrc-cnrc.gc.ca /~smd/cv.html (602 words)

	[No title]
		The star, known as GK Persei (or GK Per for short), brightens by a factor of 15 or so every three or four years, but the time of these outbursts is not exactly predictable.
		GK Per consists of a pair of stars orbiting each other at a separation of 2 million miles once every 2 days.
		Stars like GK Per are believed to undergo classical nova outbursts every 10,000 years although GK Per may be unique as it is thought the 1901 explosion may have been the first by this pair of stars.
	heasarc.gsfc.nasa.gov /docs/xte/whatsnew/ras_press_release.txt (897 words)

	The 2002 Outburst of GK Persei
		The 2002 outburst of GK Per is currently in its last stages.
		The unfolded spectrum of GK Per from the fourth observation; the best fit simple continuum model is identical to that for the third (green).
		The unfolded spectrum of GK Per from the twelfth observation, still strong in the X-rays despite the optical decline.
	lheawww.gsfc.nasa.gov /~mukai/iphome/news/gkper2002/gk2002.html (1444 words)

	[No title]
		GK Per is a remarkable close binary system, containing a white dwarf and an evolved companion of spectral type K0 IV.
		GK Per is also a remarkable system in that it has the largest measured orbital period among the classical CVs and that it has now, after its nova outburst in 1901, entered a phase characterized by occasional dwarf nova outbursts.
		In the infrared, as seen by IRAS, GK Per exhibits a region of elongated emission that is attributed to circumstellar dust.
	www.astro.su.se /~fredrik/projects.html (1927 words)

	APOD: July 4, 1998 - The Firework Nebula
		In a nova, a nuclear detonation on the surface of a compact white dwarf star blasts away material that has been dumped on its surface by a companion star.
		Persei, this nova became one of the brightest stars in the night sky in the year 1901.
		GK Per undergoes minor outbursts every three or four years.
	antwrp.gsfc.nasa.gov /apod/ap980704.html (119 words)

	AAVSO: GK Per, November 2000 Variable Star Of The Month
		Once GK Per's magnetic nature was discovered, it was classified based on the strength of the white dwarf's magnetic field into the cataclysmic variable subtype, intermediate polar or DQ Her star.
		In the course of a dwarf nova like eruption of GK Per in 1978, Andrew King and his colleagues at Leicester University were the first to discover (with the Ariel 5 satellite) that GK Persei had flared in X-rays.
		In the year 1901, after GK Persei underwent its classical nova outburst, there was a discovery that excited the astronomical community of the day.
	www.aavso.org /vstar/vsotm/1100.stm (2163 words)

	A multiwavelength study of the remnant of nova GK Persei (Site not responding. Last check: 2007-10-24)
		A multiwavelength study of the remnant of nova GK Persei
		We present new observations of the nebular remnant of the old nova GK Persei 1901 in the optical using the Himalayan Chandra Telescope (HCT) and at low radio frequencies using the Giant Metrewave Radio Telescope (GMRT).
		The nova remnant of GK Per is detected at all the observed radio frequencies and is of a similar extent to the optical remnant.
	www.edpsciences.org /articles/aa/abs/2005/19/aa2371-04/aa2371-04.html (447 words)

	Special Stars: Nova Persei 1901 (GK Persei)
		The double star GK Persei is an unusual nova star.
		Both partners are relative far away from each other, which makes a flowing of matter from the bigger partner to the White Dwarf (B) difficult.
		The Firework Nebula and GK Persei A in the center.
	jumk.de /astronomie/special-stars/nova-persei.shtml (156 words)

	Summary of sequence number 300089
		GK Persei is an extraordinary object: the first nova of the last century, it contains a magnetic white dwarf, an evolved secondary, and a large truncated accretion disk.
		The nature of the low-energy excess is not known, but it is expected to consist of a mixture of thermal emission lines from the accretion column and fluorescent emission lines from the white dwarf surface and accretion disk.
		We propose to obtain two Chandra HETG observations of GK Per in outburst to determine the nature of the low-energy emission, measure the Fe K emission line strengths, and search for other emission lines, thereby constraining the accretion geometry and the plasma conditions (range of temperatures, abundances, and density) of the X-ray--emitting plasma.
	asc.harvard.edu /cgi-gen/mp/target.cgi?300089 (171 words)

	Nova Persei 1901 (GK Persei)
		The nova returned to its minimum state – magnitude 13 – eleven years after it shot to prominence.
		From 1966 to the present, Nova Persei (now more commonly called GK Persei) has shown dwarf-nova-like outbursts of about 3 magnitudes every 3 years.
		Around 1980, the discovery of X-rays coming from this system led scientists to reclassify the system as a DQ Herculis star or intermediate polar.
	www.daviddarling.info /encyclopedia/N/Nova_Persei_1901.html (223 words)

	[No title] (Site not responding. Last check: 2007-10-24)
		This is the first detection of a nova shell in x-rays.
		The x-ray nebula extends 46" southwest, 60" northwest, 52" southeast, and 43" northeast of GK Per, with an elliptical shape.
		The shell shows a clumpy morphology with several knots that are centrally bright and limb-darkened.
	earn.dlr.de /dionysus/iauc6680.txt (243 words)

	Best of AOP: GK Persei: Nova Persei 1901
		Shown here is the nova shell of GK Persei (in the constellation of Perseus around 1,500 light years away).
		However, for whatever reason, GK Persei built up enough gas in its disk to detonate back in 1901.
		At its maximum GK Persei ranked among the brightest stars in the sky and the expanding gas reached velocities of 1200 km/s.
	www.noao.edu /outreach/aop/observers/GKper.html (311 words)

	Three-Dimensional Fabry-Perot Imaging of Filamentary Structures in Cas A and Nova GK Persei (Site not responding. Last check: 2007-10-24)
		Three-Dimensional Fabry-Perot Imaging of Filamentary Structures in Cas A and Nova GK Persei
		Previous two-dimensional spectroscopy of Cas A and Nova GK Persei has shown that these objects have significant asymmetries and anisotropies in their filamentary structures, velocity fields and elemental abundance distributions.
		For Nova GK Persei, a model was constructed from $\hbox{H} \alpha\ +$ [NII] $\lambda\lambda$6548, 6583 emission with a resolution of 150 km $\hbox{s}^{-1}$.
	www.aas.org /publications/baas/v25n2/aas182/abshtml/S213.html (216 words)

	[No title]
		Norwegian Astronomical Society - Variable Star Section *** V and B-V Sequence for Nova Type Variable Star GK Persei *** Compiled by Bjorn H. Granslo (version 2004 October 8) 0324+43 GK Per [R.A. = 03h31m12s.0, Decl.
		= +43o54o15" (2000.0)] GK Per = Nova Persei 1901 = HD 21629 = BD +43 0740a = GSC 2874-0922: This object is of type NA+XP and magnitude 0.2 - 14.0 v [GCVS].
		Sumner B., Henden A.: V and B-V sequence for GK Persei [HeSu].
	www.astro.uio.no /~bgranslo/sequence/GK_Per.seq (668 words)

	On the nature of the X-ray source in GK Persei (Site not responding. Last check: 2007-10-24)
		On the nature of the X-ray source in GK Persei
		We report XMM-Newton observations of the intermediate polar (IP) GK Per on the rise to the 2002 outburst and compare them to Chandra observations during quiescence.
		The asymmetric spin light curve implies an asymmetric shape of a semi-transparent accretion curtain and we propose a model for its shape.
	www.hs.uni-hamburg.de /DE/Ins/Per/Isaacs/gkper.html (390 words)

	Dramatic change of the recurrence time and outburst parameters of the intermediate polar GK Persei (Site not responding. Last check: 2007-10-24)
		Dramatic change of the recurrence time and outburst parameters of the intermediate polar GK Persei
		This analysis has shown that the intermediate polar GK Per experienced a very striking evolution.
		Its outbursts became wider and brighter in the last five decades.
	aanda.u-strasbg.fr:2002 /articles/aa/abs/2002/06/aa1502/aa1502.html (241 words)

	High Energy Astrophysics Picture Of the Week
		A new observation by the Chandra X-ray Observatory of a classical nova called GK Persei helps answer this question.
		GK Per erupted in 1901, and the material ejected in the explosion has smacked into interstellar material, producing a shell of shocked gas which generates the X-ray emission that Chandra sees.
		The image above shows the Chandra X-ray image of the nova remnant as a false-color image; the contour lines are derived from a radio image by the Very Large Array.
	heasarc.gsfc.nasa.gov /docs/objects/heapow/archive/nebulae/gkper_chandra.html (267 words)

	GK Persei = Nova Persei 1901
		SkyView image of GK Per (see important notes).
		GK Per is a giant among Intermediate Polars, with a highly developed disk.
		We will not even attempt to list pre-1980 papers that deal exclusively with the classical nova event of 1901; see the Bode and Evans book on Classical Novae for that.
	lheawww.gsfc.nasa.gov /users/mukai/iphome/systems/gkper.html (122 words)

	[No title]
		These included the neglected BG Andromedae, AI Persei, TU Aquilae, FF Cygni and W Piscium, which I've observed for two to seven years -- long enough to learn the idiosyncrasies of each and its comparison star sequence.
		The first four were past recent maxima and down to mags 10 or 11, none behaving close to predictions.
		My last observation was a tough one: the old nova GK Persei which in early 1901 erupted to rival Capella.
	www.cfas.org /Library/varstars.txt (977 words)

	Research (Site not responding. Last check: 2007-10-24)
		--> I got my D. Phil at the university of Sussex in 1998 after spending three years studying several aspects of the dwarf novae/ intermediate polar GK Persei.
		The title of my thesis was "Spectroscopical studies of the intermediate polar GK Persei" and has been published almost completely in the form of journal papers.
		Here is a list of some people I have worked with (or I have just talked about work with) in the past (and present):
	www.astro.soton.ac.uk /~lmr/researchv2.html (1004 words)

	Fabry-Perot Imaging Spectroscopy of the Crab Nebula, Cassiopeia A, and Nova GK Persei (Site not responding. Last check: 2007-10-24)
		Fabry-Perot Imaging Spectroscopy of the Crab Nebula, Cassiopeia A, and Nova GK Persei
		[62.01D] Fabry-Perot Imaging Spectroscopy of the Crab Nebula, Cassiopeia A, and Nova GK Persei
		Spectroscopy from MDM and the Multiple Mirror Telescope shows that the knots are characterized by remarkably strong \hbox{[Ar\hskip 2trueptIII]}~$\lambda$7136 emission, possibly indicating high argon abundances or unusual excitation mechanisms; high gas temperatures are excluded.
	www.aas.org /publications/baas/v26n4/aas185/abs/S6201.html (351 words)

	Weasner's Meade ETX Site
		The most common association with this star by far is "Mirfak," which translates as "elbow of the Hero," or "Perseus Elbow." This huge and bright (4,200 more than our own sun!) star is 570 light years distant, making it one of the most remote of all 1st magnitude (it is actually magnitude 1.8) stars.
		Also known as 38 Persei, the primary ("A") component is a very slight variable although it will not be noticeable to the visual observer.
		Zeta Persei, a nice and colorful double star for most telescopes, a rapidly expanding group of associated stars and the "California Nebula," ngc1499, a 2.5-degree streak of nebulosity to the immediate north of Zeta.
	www.weasner.com /etx/ref_guides/perseus.html (6147 words)

	Balman
		Observation of the Classical Nova Shell of Nova Persei 1901 (GK Per): A Miniature Supernova Remnant
		I present the CHANDRA ACIS-S data of the classical nova shell of Nova Persei (1901).
		Implications of this observation for the standard nova theory and the comparison of the X-ray data with optical HST observations will be elaborated.
	www.astro.physik.uni-goettingen.de /outreach/CVConference/abstracts/Balman/Balman.html (267 words)

	St. Andrews Astronomy Group Preprint Server (Site not responding. Last check: 2007-10-24)
		Mapping quasi-periodic oscillations from the outbursting intermediate polar GK Persei
		We provide a kinematically-resolved analysis of 5000s QPOs found in the optical emission lines of GK Per during a dwarf nova outburst.
		These are consistent with models of reprocessing off blobs of gas orbiting within the inner accretion disc.
	star-www.st-and.ac.uk /astronomy/preprints/qpoip_abs.html (86 words)

	Astronomi ve Uzay Bilimleri Bölümü--bolum yayinlari
		O. KURUTAÇ and C. "Photoelectric Photometry of LX Persei", Acta Astronomica, 32, 425.
		C. "Photometric Observations and Analysis of the Eclipsing Binary DM Persei", AASS, 54, 193.
		O. EVREN and Z. "Photoelectric Photometry and Photometric Elements of LX Persei", ASS, 112, 273.
	astronomy.sci.ege.edu.tr /Preview/bolum_yayinlari.html (3201 words)

	Balman (Site not responding. Last check: 2007-10-24)
		The CHANDRA Observation of The First Resolved and Detected Nova Shell, the Nova Shell of GK Persei (1901)
		The nova shell of Persei (1901) was resolved and detected with the ROSAT HRI in the X-ray wavelengths with a total count rate of about 0.01
		The X-ray nebula showed evidence of existing knots/clumps which could be the result of fragmentation and condensation in the post-shock region.
	www.astropa.unipa.it /EVENTS/XRAY2000/X-ray_Astronomy/Balman2.htm (222 words)

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