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AZ Cancri
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AZ Cancri
AZ Cancri (AZ Cnc) is a M-type flare star in the constellation Cancer. It has an apparent visual magnitude of approximately 17.59.
AZ Cancri is a member of the Beehive Cluster, also known as Praesepe or NGC 2632. The spectral type of AZ Cnc is M6e, specifically M6.5Ve, and was catalogued as a flare star by Haro and Chavira in 1964 (called by them T4). AZ Cnc has also been found to be an x-ray source, with the ROSAT designations of RX J0840.4+1824 and 1RXS J084029.9+182417. The X-ray luminosity has been found to be 27.40 ergs/s
The absolute magnitude of the star has been found to be 16.9, and thus its luminosity is approximately 3.020 × 1030 ergs/s.[citation needed]
AZ Cancri is located approximately 14.0 parsecs (46 ly) from the Sun, and is considered a very low-mass star with a radial velocity of 64.2±0.6 km/s. AZ Cancri belongs kinematically to the old disk. It is rotating at approximately 7.9±2.8 km/s.
The X-ray luminosity of AZ Cnc increased by at least two orders of magnitude during a flare that lasted more than 3 hours and reached a peak emission level of more than 1029 ergs/s. During another long duration flare (March 14, 2002) on AZ Cnc, very strong wing asymmetries occurred in all lines of the Balmer series and all strong He I lines, but not in the metal lines.
The flaring atmosphere of AZ Cancri has been analysed with a stellar atmosphere model, and was found to consist of
For the underlying photosphere, the effective temperature was found to be 2825 K, and a solar chemical composition was used. The last spectrum taken in the series after the flare was used for the quiescent chromosphere.
The line asymmetries have been attributed to downward moving material, specifically a series of flare-triggered downward moving chromospheric condensations, or chromospheric downward condensations (CDC)s as on the Sun.
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AZ Cancri
AZ Cancri (AZ Cnc) is a M-type flare star in the constellation Cancer. It has an apparent visual magnitude of approximately 17.59.
AZ Cancri is a member of the Beehive Cluster, also known as Praesepe or NGC 2632. The spectral type of AZ Cnc is M6e, specifically M6.5Ve, and was catalogued as a flare star by Haro and Chavira in 1964 (called by them T4). AZ Cnc has also been found to be an x-ray source, with the ROSAT designations of RX J0840.4+1824 and 1RXS J084029.9+182417. The X-ray luminosity has been found to be 27.40 ergs/s
The absolute magnitude of the star has been found to be 16.9, and thus its luminosity is approximately 3.020 × 1030 ergs/s.[citation needed]
AZ Cancri is located approximately 14.0 parsecs (46 ly) from the Sun, and is considered a very low-mass star with a radial velocity of 64.2±0.6 km/s. AZ Cancri belongs kinematically to the old disk. It is rotating at approximately 7.9±2.8 km/s.
The X-ray luminosity of AZ Cnc increased by at least two orders of magnitude during a flare that lasted more than 3 hours and reached a peak emission level of more than 1029 ergs/s. During another long duration flare (March 14, 2002) on AZ Cnc, very strong wing asymmetries occurred in all lines of the Balmer series and all strong He I lines, but not in the metal lines.
The flaring atmosphere of AZ Cancri has been analysed with a stellar atmosphere model, and was found to consist of
For the underlying photosphere, the effective temperature was found to be 2825 K, and a solar chemical composition was used. The last spectrum taken in the series after the flare was used for the quiescent chromosphere.
The line asymmetries have been attributed to downward moving material, specifically a series of flare-triggered downward moving chromospheric condensations, or chromospheric downward condensations (CDC)s as on the Sun.
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