Long-Term X-Ray Spectral Variability of the Nucleus of M81

Giovanni Peres, Kim, Nicastro, Fabbiano, Elvis, Giovanni Peres, La Parola

Risultato della ricerca: Article

11 Citazioni (Scopus)

Abstract

We have analyzed the soft X-ray emission from the nuclear source of the nearby spiral galaxy M81, using the available data collected with ROSAT, ASCA, BeppoSAX, and Chandra. The source flux is highly variable (sometimes dramatic: a factor of 4 in 20 days), showing variability at different timescales, from 2 days to 4 yr, and in particular a steady increase of the flux by a factor of greater than or similar to2 over 4 yr, broken by rapid flares. After accounting for the extended component resolved by Chandra, the nuclear soft X-ray spectrum (from ROSAT/PSPC, BeppoSAX/LECS, and Chandra data) cannot be fitted well with a single absorbed power-law model. Acceptable fits are obtained by adding an extra component, either a multicolor blackbody (MCBB) or an absorption feature. In the MCBB case, the inner accretion disk would be far smaller than the Schwartzchild radius for the 3-60x10(6) M-circle dot nucleus, requiring a strictly edge-on inclination of the disk, even if the nucleus is a rotating Kerr black hole. The temperature is 0.27 keV, larger than expected from the accretion disk of a Schwartzchild black hole but consistent with that expected from a Kerr black hole. In the power law+absorption feature model, we have either high-velocity (0.3c) infalling C V clouds or neutral C I absorption at rest. In both cases the C:O overabundance is a factor of 10.
Lingua originaleEnglish
pagine (da-a)831-844
Numero di pagine14
RivistaTHE ASTROPHYSICAL JOURNAL
Volume601
Stato di pubblicazionePublished - 2004

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nuclei
power law
accretion
accretion disks
x rays
spiral galaxies
flares
inclination
timescale
radii
temperature

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cita questo

Peres, G., Kim, Nicastro, Fabbiano, Elvis, Peres, G., & La Parola (2004). Long-Term X-Ray Spectral Variability of the Nucleus of M81. THE ASTROPHYSICAL JOURNAL, 601, 831-844.

Long-Term X-Ray Spectral Variability of the Nucleus of M81. / Peres, Giovanni; Kim; Nicastro; Fabbiano; Elvis; Peres, Giovanni; La Parola.

In: THE ASTROPHYSICAL JOURNAL, Vol. 601, 2004, pag. 831-844.

Risultato della ricerca: Article

Peres, G, Kim, Nicastro, Fabbiano, Elvis, Peres, G & La Parola 2004, 'Long-Term X-Ray Spectral Variability of the Nucleus of M81', THE ASTROPHYSICAL JOURNAL, vol. 601, pagg. 831-844.
Peres G, Kim, Nicastro, Fabbiano, Elvis, Peres G e altri. Long-Term X-Ray Spectral Variability of the Nucleus of M81. THE ASTROPHYSICAL JOURNAL. 2004;601:831-844.
Peres, Giovanni ; Kim ; Nicastro ; Fabbiano ; Elvis ; Peres, Giovanni ; La Parola. / Long-Term X-Ray Spectral Variability of the Nucleus of M81. In: THE ASTROPHYSICAL JOURNAL. 2004 ; Vol. 601. pagg. 831-844.
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abstract = "We have analyzed the soft X-ray emission from the nuclear source of the nearby spiral galaxy M81, using the available data collected with ROSAT, ASCA, BeppoSAX, and Chandra. The source flux is highly variable (sometimes dramatic: a factor of 4 in 20 days), showing variability at different timescales, from 2 days to 4 yr, and in particular a steady increase of the flux by a factor of greater than or similar to2 over 4 yr, broken by rapid flares. After accounting for the extended component resolved by Chandra, the nuclear soft X-ray spectrum (from ROSAT/PSPC, BeppoSAX/LECS, and Chandra data) cannot be fitted well with a single absorbed power-law model. Acceptable fits are obtained by adding an extra component, either a multicolor blackbody (MCBB) or an absorption feature. In the MCBB case, the inner accretion disk would be far smaller than the Schwartzchild radius for the 3-60x10(6) M-circle dot nucleus, requiring a strictly edge-on inclination of the disk, even if the nucleus is a rotating Kerr black hole. The temperature is 0.27 keV, larger than expected from the accretion disk of a Schwartzchild black hole but consistent with that expected from a Kerr black hole. In the power law+absorption feature model, we have either high-velocity (0.3c) infalling C V clouds or neutral C I absorption at rest. In both cases the C:O overabundance is a factor of 10.",
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AU - Fabbiano, null

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AU - Peres, Giovanni

AU - La Parola, null

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N2 - We have analyzed the soft X-ray emission from the nuclear source of the nearby spiral galaxy M81, using the available data collected with ROSAT, ASCA, BeppoSAX, and Chandra. The source flux is highly variable (sometimes dramatic: a factor of 4 in 20 days), showing variability at different timescales, from 2 days to 4 yr, and in particular a steady increase of the flux by a factor of greater than or similar to2 over 4 yr, broken by rapid flares. After accounting for the extended component resolved by Chandra, the nuclear soft X-ray spectrum (from ROSAT/PSPC, BeppoSAX/LECS, and Chandra data) cannot be fitted well with a single absorbed power-law model. Acceptable fits are obtained by adding an extra component, either a multicolor blackbody (MCBB) or an absorption feature. In the MCBB case, the inner accretion disk would be far smaller than the Schwartzchild radius for the 3-60x10(6) M-circle dot nucleus, requiring a strictly edge-on inclination of the disk, even if the nucleus is a rotating Kerr black hole. The temperature is 0.27 keV, larger than expected from the accretion disk of a Schwartzchild black hole but consistent with that expected from a Kerr black hole. In the power law+absorption feature model, we have either high-velocity (0.3c) infalling C V clouds or neutral C I absorption at rest. In both cases the C:O overabundance is a factor of 10.

AB - We have analyzed the soft X-ray emission from the nuclear source of the nearby spiral galaxy M81, using the available data collected with ROSAT, ASCA, BeppoSAX, and Chandra. The source flux is highly variable (sometimes dramatic: a factor of 4 in 20 days), showing variability at different timescales, from 2 days to 4 yr, and in particular a steady increase of the flux by a factor of greater than or similar to2 over 4 yr, broken by rapid flares. After accounting for the extended component resolved by Chandra, the nuclear soft X-ray spectrum (from ROSAT/PSPC, BeppoSAX/LECS, and Chandra data) cannot be fitted well with a single absorbed power-law model. Acceptable fits are obtained by adding an extra component, either a multicolor blackbody (MCBB) or an absorption feature. In the MCBB case, the inner accretion disk would be far smaller than the Schwartzchild radius for the 3-60x10(6) M-circle dot nucleus, requiring a strictly edge-on inclination of the disk, even if the nucleus is a rotating Kerr black hole. The temperature is 0.27 keV, larger than expected from the accretion disk of a Schwartzchild black hole but consistent with that expected from a Kerr black hole. In the power law+absorption feature model, we have either high-velocity (0.3c) infalling C V clouds or neutral C I absorption at rest. In both cases the C:O overabundance is a factor of 10.

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