Luminous blue variable P CygniP Cygni is widely considered to be the earliest known example of a luminous blue variable. However, it is far from a typical example. Typically, LBVs change in brightness with a period of years to decades, o… See more
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- Learn more:✕This summary was generated using AI based on multiple online sources. To view the original source information, use the "Learn more" links.A feature in a spectrum that indicates a strong outflow of matter from a star. It is named after P Cygni, a Be star whose spectrum shows strong hydrogen and helium emission lines with absorption lines on their blueward side.www.oxfordreference.com/display/10.1093/oi/autho…These 'P-Cygni' lines are a characteristic common to all novae and stars with strong mass ejections or violent stellar winds such as Eta Carinae. The stellar 'ashes' that accumulate often take the form of a circumstellar nebula of gas and dust.laserstars.org/spectra/PCygni.htmlA P Cygni profile is a combination of features in a star's spectrum that points to an outflow of material in the form of either an expanding shell of gas or a powerful stellar wind. The P Cygni profile is characterized by strong emission lines with corresponding blueshifted absorption lines.www.daviddarling.info/encyclopedia/P/P_Cygni_pr…A P Cygni profile is an emission spectral line shape that shows an adjacent, slightly- blueshifted (i.e., slightly shorter wavelength) absorption line.astro.vaporia.com/start/pcygniprofile.htmlP Cygni gives its name to a type of spectroscopic feature called a P Cygni profile, where the presence of both absorption and emission in the profile of the same spectral line indicates the existence of a gaseous envelope expanding away from the star.en.wikipedia.org/wiki/P_Cygni
Identification of Spectral Lines - History of P-Cygni lines
In the late 19th century, Keeler discovers the unusual emission lines of P-Cygni, a variable star which may have had a novae phase in 1600. It had several bright lines ascribed to helium , and is now classified as a very slow nova.
P Cygni - aavso
The lines show the classic "P Cygni profile" of emission on the longer-wavelength side of the line, and absorption on the shorter-wavelength side. The H-α line is centered at a wavelength of 6563 Angstroms in the rest frame.
P Cygni profile - David Darling
A P Cygni profile is a combination of features in a star's spectrum that points to an outflow of material in the form of either an expanding shell of gas or a powerful stellar wind. The P Cygni …
P Cygni profile - astro.vaporia.com
A P Cygni profile is an emission spectral line shape that shows an adjacent, slightly-blueshifted (i.e., slightly shorter wavelength) absorption line. The emission line indicates some thin …
The classic P Cygni profile consists of a broad intense emission line together with a less intense and somewhat narrower absorption line displaced to the blue side of the emission line.
An analysis of emission lines in the spectrum of P …
Sep 30, 1997 · High signal-to-noise observations of hydrogen-and helium-line profiles in the spectrum of P Cyg show a new feature— broad weak emission wings extending to ± 1500 km s⁻¹ from the line center.
P-Cygni (A hot supergiant star with powerful stellar winds where …
Sep 20, 2024 · Emission lines are characterized by the spikes in the continuum. Note: Thank you RL for correcting the description of P-Cygni.
P-Cygni Profile (Robert Eder) - AstroBin
The P-Cygni profile of a spectral line is created by a stellar wind and is characterized by a broad, unshifted emission line, which is bounded on the blue side by a narrow, blue-shifted absorption line (marked in the yellow circle).
The H-alpha Variations of the Luminous Blue Variable P Cygni: …
Jan 22, 2011 · Here we present new high resolution H-alpha spectroscopy of P Cyg that we combine with earlier spectra and concurrent V-band photometry to document the emission and …
P Cygni profiles atop broad emission lines - Oxford Academic
May 21, 1999 · In this paper we approach the problem of P Cygni profiles atop broad emission lines from a purely theoretical point of view. The line transfer in a two-winds structure is solved …
P Cygni - Astronomy Magazine
Jan 1, 2024 · P Cygni’s strong winds, however, form expanding shells that show up like fingerprints in the star’s spectrum as an odd pairing of adjacent emission and absorption …
We present a high-resolution (R ≃ 20,000) near-infrared (9,100–13,500 ˚A) long-slit spectrum of P Cygni obtained with the newly commissioned WINERED spectrograph in Japan.
A newly identified emission-line region around P Cygni - Oxford …
Aug 18, 2018 · We present a high-resolution (R ≃ 20 000) near-infrared (9100–13 500Å) long-slit spectrum of P Cygni obtained with the newly commissioned WINERED spectrograph in Japan.
P Cygni profiles atop broad emission lines - IEEE Xplore
In a normal P Cygni profile, an expanding atmosphere absorbs continuum photons from an inner core, leading to the well-known blue absorption + red emission pattern. In this paper we …
While most stars like P Cygni have a line profile that show emission lines (from elements such as hydrogen, helium, and beyond) P Cygni showed absorption lines in the bluer wavelengths and …
P Cygni stars - Astrosurf
P Cygni stars lines shows a profile type called "P Cyg": an emission component to the red side of an aborption line. There are blue super-giant stars. They have larges masses and high …
Title: A newly-identified emission-line region around P Cygni
Aug 14, 2018 · Abstract: We present a high-resolution ($R \simeq 20,000$) near-infrared (9,100-13,500 $Å$) long-slit spectrum of P Cygni obtained with the newly commissioned WINERED …
P Cygni line profile - Oxford Reference
A feature in a spectrum that indicates a strong outflow of matter from a star. It is named after P Cygni, a Be star whose spectrum shows strong hydrogen and helium emission lines with …
Intensity interferometry of P Cygni in the H$α$ emission line: …
Oct 18, 2019 · We present intensity interferometry of the luminous blue variable P Cyg in the light of its H$α$ emission performed with 1\,m-class telescopes. We compare the measured …
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