AZ Cancri

AZ Cancri is a member of the Beehive Cluster, also known as Praesepe or NGC 2632. The spectral type of AZ Cnc is M6e,{{cite journal |doi=10.1086/191611 |author1=Kirkpatrick, J. Davy |author2=Henry, Todd J. |author3=McCarthy, Donald W. Jr. |title=A standard stellar spectral sequence in the red/near-infrared - Classes K5 to M9 |journal=Astrophysical Journal Supplement |date=1991 |volume=77 |pages=417 |bibcode=1991ApJS...77..417K|doi-access=free }} specifically M6.5Ve,{{cite journal |author1=Dahn, C. |author2=Green, R. |author3=Keel, W. |author4=Hamilton, D. |author5=Kallarakal, V. |author6=Liebert, James |title=The Absolute Magnitude of the Flare Star AZ Cancri (LHS 2034) |journal=Information Bulletin on Variable Stars |date=Sep 1985 |volume=2796 |issue=1 |pages=1–2 |bibcode=1985IBVS.2796....1D }} and was catalogued as a flare star by Haro and Chavira in 1964 (called by them T4).{{cite journal|last=Bidelman|first=W. P.|author2=D. Hoffleit |title=The Absolute Magnitude of AZ Cancri|journal=Information Bulletin on Variable Stars|year=1983|volume=2414|issue=1|page=1|bibcode=1983IBVS.2414....1B}}{{ cite journal |vauthors=Haro G, Chavira E, Gonzalez G |title=Flare stars in the Praesepe field |journal=Bol Inst Tonantzintla. |date=Dec 1976 |volume=2 |issue=12 |pages=95–100 |bibcode=1976BITon...2...95H }} 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{{ cite journal |author1=Fleming TA |author2=Giampapa MS |author3=Schmitt JHMM |author4=Bookbinder JA |title=Stellar coronae at the end of the main sequence - A ROSAT survey of the late M dwarfs |journal=Astrophys. J. |date=Jun 1993 |volume=410 |issue=1 |pages=387–92 |doi=10.1086/172755 |bibcode=1993ApJ...410..387F |doi-access=free }}

The absolute magnitude of the star has been found to be 16.9, and thus its luminosity is approximately 3.020 x 10³⁰ ergs/s.{{citation needed|date=July 2014}}

AZ Cancri is located approximately {{convert|14.0|pc|ly}} from the Sun, and is considered a very low-mass star{{ cite journal |doi=10.1086/116091 |vauthors=Monet DG, Dahn CC, Vrba FJ, Harris HC, Pier JR, Luginbuhl CB, Ables HD |title=U.S. Naval Observatory CCD parallaxes of faint stars. I - Program description and first results |journal=Astron. J. |date=1992 |volume=103 |pages=638 |bibcode=1992AJ....103..638M|doi-access=free }} 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.

{{see also|flare star}}

File:AZCncLightCurve.png light curve for a flare on AZ Cancri, adapted from Fuhrmeister et al. (2005)]]

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.{{ cite journal |author1=Fuhrmeister B |author2=Schmitt JHMM |author3=Hauschildt PH |title=Detection of red line asymmetries in LHS 2034 |journal=Astron. Astrophys. |date=Jun 2005 |volume=436 |issue=2 |pages=677–86 |doi=10.1051/0004-6361:20042518 |bibcode=2005A&A...436..677F|doi-access=free }}

The flaring atmosphere of AZ Cancri has been analysed with a stellar atmosphere model,{{ cite journal |vauthors=Hauschildt PH, Allard F, Baron E |title=The NextGen Model Atmosphere Grid for 3000<=T_eff<=10,000 K |journal=Astrophys. J. |date=Feb 1999 |volume=512 |issue=1 |pages=377–85 |bibcode=1999ApJ...512..377H |doi=10.1086/306745 |arxiv = astro-ph/9807286 |s2cid = 16132773}} and was found to consist of

1. an underlying photosphere,
2. a linear temperature rise vs. log column mass in the chromosphere, and
3. transition region (TR) with different gradients.

For the underlying photosphere, the effective temperature was found to be 2800 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.{{ cite journal |author=Fisher GH |title=Dynamics of flare-driven chromospheric condensations |journal=Astrophys. J. |date=Nov 1989 |volume=346 |issue=11 |pages=1019–29 |bibcode=1989ApJ...346.1019F |doi=10.1086/168084 |doi-access=free }}

The electrodynamic coupling theory of coronal heating developed in a solar context,{{ cite journal |author=Ionson J |journal=Astrophys. J. |date=1984 |volume=276 |pages=357 |doi=10.1086/161620 | bibcode=1984ApJ...276..357I | title=A unified theory of electrodynamic coupling in coronal magnetic loops - The coronal heating problem |doi-access=free }} has been applied to stellar corona.{{ cite journal |doi=10.1086/162239 |author=Mullan DJ |title= On the possibility of resonant electrodynamic coupling in the coronae of red dwarfs|journal=Astrophys. J. |date=1984 |volume=282 |pages=603 |bibcode=1984ApJ...282..603M}} A distinctive feature is the occurrence of a resonance between the convective turnover time and the crossing time for Alfvén waves in a coronal loop. The resonance attains a maximum among the early M dwarf spectral types and declines thereafter. A turnover in coronal heating efficiency, presumably manifested by a decrease in L_x/L_bol, becomes evident toward the late M spectral types when the theory is applicable. This is consistent with an apparent lack of X-ray emission among the late M dwarfs.{{Cite thesis |last=Bookbinder |first=J. A. |title=Observations of non-thermal radiation from late-type stars |date=1985 |publisher=Harvard University |location=Cambridge, MA |bibcode=1985PhDT........13B }} Coronal heating efficiencies do not decrease toward the presumably totally convective stars near the end of the main sequence. For "saturated" M dwarfs, 0.1% of all energy is typically radiated in X-rays, while for AZ Cnc this number increases during flaring to 7%. So far there is no evidence to suggest that AZ Cnc is less efficient than more massive dwarfs in creating a corona. The saturation boundary in X-ray luminosity extends to late M dwarfs, with L_x/L_bol ~ 10⁻³ for saturated dwarfs outside flaring. No coronal dividing line exists in the Hertzsprung–Russell diagram at the low-mass end of the main sequence.

AZ Cnc casts doubt on the applicability of electrodynamic coupling as there is no evidence for a sharp drop in L_x/L_bol when compared with other late M stars at least until subtype M8.

AZ Cnc has a corona and this may indicate that a distributive dynamo is just as efficient in producing magnetic flux as a shell dynamo. Between the generation of a magnetic field and the emission of X-rays lies the coronal heating mechanism.

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{{Stars of Cancer}}

{{DEFAULTSORT:AZ Cancri}}

Category:Astronomical X-ray sources

Category:Cancer (constellation)

Category:Flare stars

Category:M-type main-sequence stars

Cancri, AZ

Category:TIC objects