the dacs and sacs effects from stars to quasars. some first general notices e. danezis university of...
TRANSCRIPT
The DACs and SACs effectsfrom stars to Quasars.
Some first general notices
E. DanezisUniversity of Athens, Faculty of Physics,
Department of Astrophysics, Astronomy and Mechanics
In collaboration with A. Antoniou (University of Athens)E. Lyratzi (University of Athens)L. Č. Popović (Astronomical Observatory of Belgrade)M. S. Dimitrijević (Astronomical Observatory of Belgrade)
The spectral lines in astrophysical objectsIt is well known that the
absorption spectral lines that we can detect in the spectra of normal stars or normal galaxies, are an important factor to study many physical parameters of plasma surrounding these objects.
In these figures we can see two groups of classical stellar spectra of different spectral subtypes that present normal spectral absorption lines.
Two typical spectra of normal Galaxies
that present only absorption spectral lines.
However Hot Emission Stars (Oe and Be stars) present peculiar line profiles
Here we can see the comparison of Mg II resonance lines between the spectrum of a normal B star and the spectra of two active Be stars that present complex and peculiar spectral lines. In the first figure we observe a combination of an emission and some absorption components (P Cygni).
HD 37022, SWP07481
C IV λλ 1548.155, 1550.774 Ǻ
Si IV λλ 1393.755, 1402.770 Ǻ
HD 57061, SWP18949
In this figures we can see the complex structure of the C IV and Si IV UV resonance lines in the spectra of two Oe stars
Here we present the peculiar profile of C IV doublet in the UV spectrum of AGN PG 0946+301.
The two observed features do not present the two resonance lines
Some times we can detect peculiar spectral lines in AGNs spectra
In this figure we present typical spectra of many types of AGNs in the UV spectral range (Reichard et al. 2003, AJ, 126, 2594). The combination of emission and, in some cases, absorption components produce peculiar profiles (P Cygni profiles).
Peculiarity in AGN spectra
In order to explain the peculiarity of the line profiles in the spectra of hot emission stars, our team proposes and uses the DACs (Bates & Halliwell, 1986) and SACs (Danezis et al. 2005) theory.
The DACs phenomenon
In a stellar atmosphere, or disc, that we can detect around hot emission stars, an absorption line can be produced in several density regions that present the same temperature. From each one of these regions an absorption line arises.
The line profile distribution of each one of these absorption components is a function of a group of physical parameters, as the radial, the rotational, the random velocities and the optical depth of the region that produces the specific components of the spectral line.
These spectral lines are named Discrete Absorption Components (DACs) when they are discrete (Bates, B. & Halliwell, D. R.: 1986, MNRAS, 223, 673).
DACs are discrete but not unknown absorption spectral lines. They are spectral lines of the same ion and the same wavelength as a main spectral line, shifted at different Δλ, as they are created in different density regions which rotate and move radially with different velocities (Danezis et al. 2003).
DACs are lines, easily observed, in the spectra of some Be stars, because the regions that give rise to such lines, rotate with low velocities and move radially with high velocities (Danezis et al. 2005).
In these figures we can see the Mg II spectral lines of two Be stars that present DACs, in comparison with the Mg II lines of a classical B star. In these line profiles we can see the main spectral lines and at the left of each one of them a group of DACs.
It is very important to point out that we can detect the same phenomenon in the spectra of some AGNs
In this figure we can see the C IV UV doublet of an AGN (PG 0946+301).
From the values of radial displacements and the ratio of the line intensities we can detect that the two observed C IV shapes indicate the presence of a DACs phenomenon similar with the DACs phenomenon that we can detect in the spectra of hot emission stars.
The DACs arise from spherical density regions around the star, or from density regions far away from the star that present spherical (or apparent spherical) symmetry around their own center.
What is the origin of DACs phenomenon In the stellar atmospheres
or disc
In the case of AGNs, accretion, wind (jets, ejection of matter etc.), BLR (Broad Line Regions) and NLR (Narrow Line Regions) are, perhaps, the density regions that construct peculiar profiles of the spectral lines.
In the case of AGNs Spectra
Around a Wolf-Rayet star (WR 104) we can detect density regions of matter quite away from the stellar object, able to produce peculiar profiles.(This figure is taken by Tuthill, Monnier & Danchi (1999) with Keck Telescope.)
Similar phenomena can be detected as an effect of the ejected plasma around peculiar stars.
The SACs phenomenon If the regions that give rise to the DACs,
rotate with large velocities and move radially with small velocities, the produced lines have large widths and small shifts.
As a result they are blended among themselves as well as with the main spectral line and thus they are not discrete. In such a case the name Discrete Absorption Components is inappropriate and we use only the name Satellite Absorption Components (SACs) (Danezis et al. 2005).
In this figure it is clear that the Mg II line profiles of the star AX Mon (HD 45910), which presents DACs and the star HD 41335, which presents SACs are produced in the same way. The only difference between them is that the components of HD 41335 are much less shifted and thus they are blended among themselves. The black line presents the observed spectral line's profile and the red one the model's fit. We also present all the components which contribute to the observed features, separately.
In these figures we can see the SACs phenomenon in the spectra
of three Oe stars
In this figures we can see the SACs phenomenon in the spectrum
of an AGN
The proposed model
In the case of DACs or SACs phenomenon we need to calculate the line function of the complex line profile.Recently, our group proposed a model in order to explain the complex structure of the density regions of hot emission stars and some AGNs, where the spectral lines that present SACs or DACs are created (Danezis et al. 2003, 2005). The main hypothesis of this model is that the stellar envelope is composed of a number of successive independent absorbing density layers of matter and a number of emission regions.
ggi j
ejejejiifinal LLSLFF
expexp1exp)( 0
The line function
where:Ιλ0: is the initial radiation intensity,Li, Lej, Lg: are the distribution functions of the absorption coefficients kλi, kλej, kλg,ξ: is the optical depth in the centre of the spectral line,Sλej: is the source function, that is constant during the specific observation.
absorption emission General absorption
2
2
0000
0
coscos22
cos222
d
zerf
zerf
zL final
radlab 0
Vradial
Vrotation
Danezis, E., Lyratzi, E., Nikolaidis, D., Antoniou, A., Popović, L. Č. & Dimitrijević, M. S., 2007 PASJ (accepted) and SPIG 2006, Kopaonik, Serbia.
c
Vz rot
0
2ln2
c
Vrandom Gaussian standard deviation
The calculation of the parameters
Directly from the model The apparent radial velocities (Vrad) of the absorbing or emitting density regionsThe Gaussian standard deviation (σ) of the random motions distributionThe apparent rotational velocities (Vrad) of the absorbing or emitting density region.The optical depth (ξ) in the center of the spectral lineFrom the above parameters we can calculate 1. The percentage contribution (G%) of the random velocities to the broadening of the spectral line2. The FWHM 3. The random velocities of the ions (Vrandom) that produce the spectral lines4. The absorbed or emitted energy (Εa, Ee)5. The column density (CD)
We point out that with the proposed model we can study and reproduce specific spectral lines. This means that we can study specific density regions in the plasma surrounding the studied object.
Some first general results
As we know, in order to find the mechanism that is responsible for the structure of DACs or SACs density regions we need to calculate the values of a group of parameters, such as the rotational, the random and the radial velocities, the FWHM, the optical depth, the absorbed or emitted Energy, the Column Density, and the Gaussian Standard Deviation, as well as the relation among them.Another interesting point is to study the time scale variation of all the above parameters.This is the reason why we present the following applications.
A statistical study of C IV, N IV and N V regions in the spectra of 20 Oe stars
In this application we study the C IV, N IV and N V regions in the spectra of 20 Oe stars and we calculate the values of the above parameters of these regions. We also study the relation among them. At the end of this session Dr Lyratzi will present some general conclusions about the structure of Si IV, Mg II and Ha density regions in Be stars
Stars Spectral types
HD24534 O9.5 III
HD24912 O7.5 III ((f))
HD34656 O7 II (f)
HD36486 O9.5 II
HD37022 O6 Vp
HD47129 O7.5 III
HD47839 O7 III
HD48099 O6.5 V
HD49798 O6p
HD57060 O8.5If
Stars Spectral types
HD57061 O9.0I
HD60848 O8.0Vpe
HD91824 O7V((f))
HD93521 O9.5II
HD112244 O8.5Iab
HD149757 O9V(e)
HD164794 O4V((f))
HD203064 O8V
HD209975 O9.5I
HD210839 O6.0I
The studied Stars
In this table we present the studied stars. As we know it is not possible to find stars between O0 and O3 spectral subtypes.
.
With our model we calculated the random velocities of the layers that produce the C IV, NIV and NV satellite components in the spectra of 20 Oe stars, with different photospheric rotational velocities.
The ionization potential of each studied ion, for all the studied stars, is the same, so the respective random velocities will be the same.
As the values of the random velocities do not depend on the inclination of the rotational axis, we expect similar average values of the random velocities for each component for all the studied stars.
In the following figures we present the relation between the random velocities of the ions that create the C IV, N IV and N V lines in the spectra of 20 stars as a function of the photospheric rotational velocities of the studied stars
C IV regions Random Velocities for the 4th component
0
200
400
600
800
1000
0 100 200 300 400 500
Vphot (km/s)
Vra
nd
(k
m/s
)
C IV regions Random Velocities for the 3rd component
0
200
400
600
800
1000
0 100 200 300 400 500
Vphot (km/s)
Vra
nd
(k
m/s
)C IV regions
Random Velocities for the 2nd component
0
200
400
600
800
1000
0 100 200 300 400 500
Vphot (km/s)
Vra
nd
(k
m/s
)
C IV regions Random Velocities for the 1st component
0
200
400
600
800
1000
0 100 200 300 400 500
Vphot (km/s)
Vra
nd
(k
m/s
)The C IV region of 20 Oe stars
mean Vrandom = 160 km/s
mean Vrandom = 115 km/smean Vrandom = 160 km/s
mean Vrandom = 80 km/s mean Vrandom = 90 km/s
In this figures we present the random velocities (Vrand) of the ions in the C IV regions that produce the satellite components as a function of the apparent photospheric rotational velocities (Vphot). We detect similar average values of the random velocities for each component for all the studied stars
N IV regions (Gaussian way) Random Velocities for the 2nd component
0
200
400
600
800
1000
0 50 100 150 200 250 300 350 400
Vphot (km/s)
Vra
nd
(k
m/s
)
N IV regions (Gaussian way) Random Velocities for the 1st component
0
200
400
600
800
1000
0 50 100 150 200 250 300 350 400
Vphot (km/s)
Vra
nd
(k
m/s
)
In this figures we present the random velocities (Vrandom) of the N IV regions that produce the satellite components as a function of the apparent photospheric rotational velocities (Vphot). We detect similar average values of the random velocities for each component for all the studied stars
The N IV regions of 20 Oe stars
mean Vrandom = 267 km/s mean Vrandom = 133 km/s
N V regions (Rotational way) Random Velocities for the 3rd component
0
200
400
600
800
1000
1200
1400
0 100 200 300 400 500
Vphot (km/s)
Vra
nd
(k
m/s
)
N V regions (Rotational way) Random Velocities for the 2nd component
0
200
400
600
800
1000
1200
1400
0 100 200 300 400 500
Vphot (km/s)
Vra
nd
(k
m/s
)
N V regions (Rotational way) Random Velocities for the 1st component
0
200
400
600
800
1000
1200
1400
0 100 200 300 400 500
Vphot (km/s)
Vra
nd
(k
m/s
)The N V region of 20 Oe stars
mean Vrandom = 160 km/smean Vrandom = 190 km/s
mean Vrandom = 108 km/s
In this figures we present the random velocities (Vrand) of the N V regions that produce the satellite components as a function of the apparent photospheric rotational velocities (Vphot). We detect similar average values of the random velocities for each component for all the studied stars
As we see, we detect similar average values of the random velocities for each component, for the C IV, N IV and N V regions, for all the studied stars. The above results, taken with our model agree with the theory.This agreement between theory and calculations is a favourable test for our model.
Important remark
2. In the following figures we present the ratio Vrot/Vphot of the C IV, N IV and N V components as a function of the photospheric rotational velocity (Vphot).This ratio indicates how much the rotational velocity of the specific layer that construct the specific component is higher than the apparent rotational velocity of the star
Studding the Rotational Velocities of the density layers of matter
Vrot=Rotational Velocity of the studied density regionVphot=Apparent Photospheric Rotational Velocity
C IV regions Vrot/Vphot for the 3rd component
0,00
1,00
2,00
3,00
4,00
5,00
6,00
7,00
0 100 200 300 400 500
Vphot (km/s)
Vro
t/V
ph
otC IV regions
Vrot/Vphot for the 2nd component
0,00
5,00
10,00
15,00
20,00
25,00
30,00
0 100 200 300 400 500
Vphot (km/s)
Vro
t/V
ph
ot
C IV regions Vrot/Vphot for the 1st component
0,005,00
10,00
15,0020,0025,0030,00
35,0040,00
0 100 200 300 400 500
Vphot (km/s)
Vro
t/V
ph
ot
The C IV region of 20 Oe stars
max (Vrot/Vphot) = 40
max (Vrot/Vphot) = 6
max (Vrot/Vphot) = 25
In these figures we present the ratio Vrot/Vphot of the four detected components of C IV as a function of the photospheric rotational velocity (Vphot).
C IV regions Vrot/Vphot for the 4th component
0,00
1,00
2,00
3,00
4,00
5,00
6,00
0 100 200 300 400 500
Vphot (km/s)
Vro
t/V
ph
ot
max (Vrot/Vphot) = 6
N IV regions Vrot/Vphot for the 2nd component
0,00
0,50
1,00
1,50
2,00
2,50
3,00
100 120 140 160 180 200 220 240
Vphot (km/s)
Vro
t/V
ph
ot
N IV regions Vrot/Vphot for the 1st component
0,00
1,00
2,00
3,00
4,00
5,00
6,00
7,00
70 120 170 220 270 320 370 420
Vphot (km/s)
Vro
t/V
ph
otThe N IV region of 20 Oe stars
Vrot/Vphot = f(Vphot)
max (Vrot/Vphot) = 6 max (Vrot/Vphot) = 2.5
The ratio Vrot/Vphot indicates how much the rotational velocity of the specific N IV layer is higher than the apparent rotational velocity of the star
N IV regions Vrot/Vphot for the 3rd component
0,00
5,00
10,00
15,00
20,00
25,00
30,00
0 100 200 300 400 500
Vphot (km/s)
Vro
t/V
ph
ot
N IV regions Vrot/Vphot for the 2nd component
0,005,00
10,0015,0020,00
25,0030,00
35,0040,00
0 100 200 300 400 500
Vphot (km/s)
Vro
t/V
ph
ot
N IV regions Vrot/Vphot for the 1st component
0,00
10,00
20,00
30,00
40,00
50,00
0 100 200 300 400 500
Vphot (km/s)
Vro
t/V
ph
otThe N V region of 20 Oe stars
Vrot/Vphot = f(Vphot)
max (Vrot/Vphot) = 45 max (Vrot/Vphot) = 40
max (Vrot/Vphot) = 25
The ratio Vrot/Vphot indicates how much the rotational velocity of the specific N V layer is higher than the apparent rotational velocity of the star
A statistical study of the parameters of the C IV, N IV and N V regions
In this application we present (in the following figures) the values of some parameters that we can calculate studding the C IV, N IV and N V density regions of 20 Oe stars and the relations among them.
Also in three poster papers you can see the relation between all the studded parameters of C IV, N IV and N V regions and the spectral subtypes.
C IV regions σ=f(Vrad)
0
0,2
0,4
0,6
0,8
1
1,2
-3500-3000-2500-2000-1500-1000-5000
Vrad (km/s)
σ
Relation between radial velocities and Gaussian Standard Deviation
Relation between radial and random velocities
C IV regions Vrand=f(Vrad)
0
50
100
150
200
250
-3500-3000-2500-2000-1500-1000-5000
Vrad (km/s)
Vra
nd
(k
m/s
)
C IV region
Relation between radial velocities and FWHM
Relation between radial velocities and Optical Depth
C IV regionC IV regions
FWHM=f(Vrad)
0,02,04,06,08,0
10,012,014,016,0
-3500-3000-2500-2000-1500-1000-5000
Vrad (km/s)
FW
HM
C IV regions (λ 1548.155 Α) Optical depth ξ=f(Vrad)
0
0,2
0,4
0,6
0,8
1
-3500-3000-2500-2000-1500-1000-5000
Vrad (km/s)
ξ
Relation between radial and rotational velocities
Relation between radial velocities and Column Densities
C IV regionC IV regions
Vrot=f(Vrad)
0
200400
600800
1000
12001400
1600
-3500-3000-2500-2000-1500-1000-5000
Vrad (km/s)
Vro
t (k
m/s
)
C IV regions (λ 1550.774 Α) Column Density (10^10 cm^-2) CD=f(Vrad)
0,00
1,00
2,00
3,00
4,00
5,00
6,00
-3500-3000-2500-2000-1500-1000-5000
Vrad (km/s)
CD
A statistical study of the parameters of the N IV regions
Relation between radial velocities and Column Densities
Relation between radial velocities and FWHM
N IV regions Column Density (10^10 cm^-2) CD=f(Vrad)
1,5
2
2,5
3
3,5
4
4,5
-350-300-250-200-150-100-500
Vrad (km/s)
CD
N IV region
Περιοχή N IV regionsFWHM=f(Vrad)
0,00
1,00
2,00
3,00
4,00
5,00
6,00
-350-300-250-200-150-100-500
Vrad (km/s)
FW
HM
Relation between radial velocities and Gaussian Standard Deviation
Relation between radial and random velocities
N IV regionN IV regions
σ=f(Vrad)
0,00
0,50
1,00
1,50
2,00
-350-300-250-200-150-100-500
Vrad (km/s)
σ
N IV regionsVrand=f(Vrad)
0
100
200
300
400
-350-300-250-200-150-100-500
Vrad (km/s)
Vra
nd
(k
m/s
)
A statistical study of the parameters of the N V regions
Relation between radial and random velocities
Relation between radial velocities and FWHM
N V regionN V regions
Vrand=(Vrad)
0
100
200
300
400
500
600
-2600-2100-1600-1100-600-100
Vrad (km/s)
Vra
nd
(k
m/s
)
N V regionsFWHM=(Vrad)
0,0
5,0
10,0
15,0
20,0
-2600-2100-1600-1100-600-100
Vrad (km/s)
FW
HM
Relation between radial velocities and Gaussian Standard Deviation
Relation between radial velocities and Column Densities
N V regionN V regions
σ=(Vrad)
0,00
0,50
1,00
1,50
2,00
-2600-2100-1600-1100-600-100
Vrad (km/s)
σ
N V regions (λ 1238.821 Α) Column Density (10^10 cm^-2) CD=f(Vrad)
1,00
2,00
3,00
4,00
5,00
6,00
-2600-2100-1600-1100-600-100
Vrad (km/s)
CD
Relation between the radial velocities and the Rotational Velocities
N V region
N V regionsVrot=(Vrad)
0
500
1000
1500
2000
-2500-2000-1500-1000-5000
Vrad (km/s)
Vro
t (k
m/s
)
As Franco et al. (1982) and Kapper et al. (1996) indicate, the radial velocities increase from the high to the low ionization potential. Our results verify this proposition.
-2500
-2000
-1500
-1000
-500
0
Vra
d (k
m/s
)
47,448 47,887 77,472
I.P. (eV)
Radial Velocities - Ionization PotentialVrad=f(I.P)
Time scale variations of the C IV, Si IV, N IV and N V density regions in the HD 93521 stellar
atmosphere
Antoniou, A., Danezis, E., Lyratzi, E., Nikolaidis, D., Popović, L. Č., Dimitrijević, M. S., & Theodosiou, E., XXVIth IAU General Assembly, Prague, August, 2006.
In this application we present the time scale variations of the C IV, N IV, Si IV and N V regions parameters.
This is an important study to examine in a future work the mechanism that is able to construct the DACs or SACs Phenomenon
A study of the density regions that construct the C IV resonance lines λλ 1548.155, 1550.774
Åin the HD 93521 (Oe) UV spectrum
The Oe star HD 93521
In this figure we can see the complex structure of C IV UV resonance lines. Each one of them consists in five components
The Oe star HD 93521. The C IV region
C IV regions - 5th componentRotational Velocities
0
200
400
600
800
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vro
t (k
m/s
)
C IV regions - 4th componentRotational Velocities
0
200
400
600
800
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vro
t (k
m/s
)C IV regions - 3rd component
Rotational Velocities
0
200
400
600
800
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vro
t (k
m/s
)
C IV regions - 2nd componentRotational Velocities
0100200300400500600700800
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vro
t (k
m/s
)C IV regions - 1st component
Rotational Velocities
0100200300400500600700800
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vro
t (k
m/s
)
Time scale variation of Rotational Velocities (Vrot) for the five components
Vrot1 = 600 km/s, s=100 km/s
Vrot2 = 140 km/s, s=44 km/s
Vrot3 = 136 km/s, s=36 km/s
Vrot4 = 97 km/s, s=31Km/s
Vrot5 = 85 km/s, s=19 km/s
The Oe star HD 93521. The C IV region
C IV regions - 5th componentRadial Velocities
-800-700-600-500-400-300-200-100
0
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
d (
km
/s)
C IV regions - 4th componentRadial Velocities
0100200300400500600700800
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
d (
km
/s)
C IV regions - 3rd componentRadial Velocities
-800-700-600-500-400-300-200-100
0
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
d (
km
/s)
C IV regions - 2nd componentRadial Velocities
0100200300400500600700800
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
d (
km
/s)
C IV regions - 1st componentRadial Velocities
-800-700-600-500
-400-300-200-100
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
d (
km
/s)
Vrad1 =-735 km/s, s=15 km/s
Vrad2 = 112 km/s, s=22 km/s
Vrad3 = -736 km/s, s=10 km/s
Vrad4 = 269 km/s, s=7km/s
Vrad5 = -176 km/s, s=45 km/s
The Oe star HD 93521. The C IV region
Time scale variation of
Radial Velocities (Vrad) for
the five components
Here and in all the following figures, s (standard deviation) does non depend only on the statistical error but, mainly, it indicates the time scale variation of the studied values.
C IV regions - 5th componentRandom Velocities
0
100
200
300
400
500
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
nd
(k
m/s
)
C IV regions - 4th componentRandom Velocities
0
100
200
300
400
500
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
d (
km
/s)
C IV regions - 3rd componentRandom Velocities
0
100
200
300
400
500
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
nd
(k
m/s
)
C IV regions - 2nd componentRandom Velocities
0
100
200
300
400
500
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
nd
(k
m/s
)C IV regions - 1st component
Random Velocities
0
100
200
300
400
500
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
nd
(k
m/s
)
Time scale variations of Random velocities (Vrand) for the five components
Vrand1 =237 km/s, s=72 km/s
Vrand2 = 156 km/s, s=34 km/s
Vrand3 = 192 km/s, s=22 km/s
Vrand4 = 154 km/s, s=28 km/s
Vrand5 = 142 km/s, s=53 km/s
The Oe star HD 93521. The C IV region
C IV regions - 3rd componentColumn Density (10^10 cm^-2)
2,00
3,00
4,00
5,00
6,00
7,00
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
CD
C IV regions - 2nd componentColumn Density (10^10 cm^-2)
7,00
8,00
9,00
10,00
11,00
12,00
13,00
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
CD
C IV regions - 1st componentColumn Density (10^10 cm^-2)
2,00
3,00
4,00
5,00
6,00
7,00
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
CD
Time scale variation of Column Density for the five components (1010 cm-2)
The Oe star HD 93521. The C IV region
C IV regions - 4th componentColumn Density (10^10 cm^-2)
4,00
5,00
6,00
7,00
8,00
9,00
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
CD
C IV regions - 5th componentColumn Density (10^10 cm^-2)
0,500,700,901,101,301,501,701,902,10
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
CD
A study of the density regions that construct the N IV spectral line λ 1718.8 Å
in the HD 93521 (Oe) UV spectrum
The Oe star HD 93521. The N IV region
The N IV line is a simple spectral line that we can feet with a Gaussian
The Oe star HD 93521. The N IV region
N IV regionsRadial velocities
-800-700-600-500-400-300-200-100
0
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
d (
km
/s) Vrad = -97 km/s s=22 km/s
The Oe star HD 93521. The N IV region
Time scale variation of Radial Velocities (Vrad, km/s)
N IV regions Random velocities
0
50
100
150
200
250
300
350
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
nd
(k
m/s
)
Vrand = 160 km/s s=19 km/s
The Oe star HD 93521. The N IV region
Time scale variation of random velocities (Vrand, km/s)
N IV regionsColumn Density (10^10 cm^-2)
0
0,2
0,4
0,6
0,8
1
1,2
1,4
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
CD
Time scale variation of the Column Density (1010 cm-2)
The Oe star HD 93521. The N IV region
The density regions that construct the N V resonance lines λλ 1238.821, 1242.804 Å in
the HD 93521 (Oe) UV spectrum
The Oe star HD 93521. The N V region
The Oe star HD 93521. The N V region
The N V resonance lines consist in an absorption and an emission component. We can feet each one of them with a Gaussian
N V regions (absorption)Radial velocities
-800
-600
-400
-200
0
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
d (
km
/s)
Time scale variation of the absorption component radial velocities (Vrad, km/s)
Vrad = -209 km/s s=34 km/s
The Oe star HD 93521. The N V region
N V regions (absorption)Random velocities
0
50
100
150
200
250
300
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
nd
(k
m/s
)
Time scale variation of the absorption component random velocities (Vrand, km/s)
Vrand = 238 km/s s=34 km/s
The Oe star HD 93521. The N V region
N V regions (absorption λ 1238.821 Α) Column Density (10^10 cm^-2)
0
0,5
1
1,5
2
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
CD
Time scale variation of the absorption component Column Density (1010 cm-2)
The Oe star HD 93521. The N V region
N V regions (emission) Radial velocities
0
200
400
600
800
1000
1200
1400
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
d (
km
/s)
Vrad = 1095 km/s s=68 km/s
The Oe star HD 93521. The N V region
Time scale variation of the emission component radial velocities (Vrad, km/s)
N V region (emission) Random velocities
0
100
200
300
400
500
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
Vra
nd
(k
m/s
)
Time scale variation of the emission component random velocities (Vrand, km/s)
Vrand = 302 km/s s=50 km/s
The Oe star HD 93521. The N V region
N V region (emission λ 1238.821 Α) Column Density (10^10 cm^-2)
0
0,5
1
1,5
2
1978 1980 1982 1984 1986 1988 1990 1992 1994 1996
Year
CD
Time scale variation of the emission component Column density (1010 cm-2)
The Oe star HD 93521. The N V region
The density regions that construct the UV Si IV resonance lines λλ 1393.755, 1402.770 Å
in the HD 93521 (Oe) UV spectrum
The Oe star HD 93521. The Si IV region
The Oe star HD 93521. The Si IV region
In this figure we can see the complex structure of UV Si IV resonance lines. Each one of them consists in three components
Si IV regions (2nd component)Rotational Velocities
0
100
200
300
400
500
600
1975 1980 1985 1990 1995 2000
Year
Vro
t (k
m/s
)
Si IV regions (1st component)Rotational Velocities
0
100
200
300
400
500
600
1975 1980 1985 1990 1995 2000
Year
Vro
t (k
m/s
)
Si IV regions (3rd component)Rotational Velocities
0
100
200
300
400
500
600
1975 1980 1985 1990 1995 2000
Year
Vro
t (k
m/s
)
Time scale variations of Rotational Velocities (Vrot) for the three components
Vrot1=410 km/s, s=120 km/s
Vrot3=205 km/s, s=40 km/s
The Oe star HD 93521. The Si IV region
Vrot2=230 km/s, s=103 km/s
Si IV regions (3rd component)Radial Velocities
-350
-300
-250
-200
-150
-100
-50
0
1975 1980 1985 1990 1995 2000
Year
Vra
d (
km
/s)
Si IV regions (2nd component)Radial Velocities
-350
-300
-250
-200
-150
-100
-50
0
1975 1980 1985 1990 1995 2000
Year
Vra
d (
km
/s)
Si IV regions (1st component)Radial Velocities
-350
-300
-250
-200
-150
-100
-50
0
1975 1980 1985 1990 1995 2000
Year
Vra
d (
km
/s)
Time scale variations of Radial Velocities (Vrad) forthe three components
Vrad1=-262 km/s, s=21 km/s Vrad2=-222 km/s, s=27 km/s
Vrad3=-217 km/s, s=50 km/s
The Oe star HD 93521. The Si IV region
Si IV regions (2nd component)Random Velocities
050
100150200
250300
350400
1975 1980 1985 1990 1995 2000
Year
Vra
nd
(k
m/s
)
Si IV regions (1st component)Random Velocities
050
100150
200250
300350
400
1975 1980 1985 1990 1995 2000
Year
Vra
nd
(k
m/s
)
Si IV regions (3rd component)Random Velocities
0
50100
150200
250
300350
400
1975 1980 1985 1990 1995 2000
Year
Vra
nd
(k
m/s
)
Time scale variations of Randon velocities (Vrand) for the three components
Vrand1=195 km/s, s=72 km/s Vrand2=109 km/s, s=50 km/s
Vrand3=82 km/s, s=13 km/s
The Oe star HD 93521. The Si IV region
Time scale variations of Column Density for the five components (1010 cm-2)
The Oe star HD 93521. The Si IV regionSi IV regions (1st component)
Column Density (10^10 cm^-2)
0,00
1,00
2,00
3,00
4,00
5,00
6,00
1975 1980 1985 1990 1995 2000
Year
CD
Si IV regions (2nd component)Column Density (10^10 cm^-2)
0,00
1,00
2,00
3,00
4,00
5,00
6,00
1975 1980 1985 1990 1995 2000
Year
CD
Si IV regions (3rd component)Column Density (10^10 cm^-2)
0,00
0,50
1,00
1,50
2,00
2,50
3,00
3,50
1975 1980 1985 1990 1995 2000
Year
CD
Fitting some AGNs spectral lines
The present work of our scientific group is to study the complex structure of some AGNs spectral lines with the proposed model in order to understand the origin of DACs and SACs phenomena.Some days before, Dr Chatzichristou presented some first ideas about this problemIn the following figures we present fits of some AGNs complex spectral lines.
3C351 CIV λ1548.187
λ 1550.772
The fit of C IV resonance lines (λλ 1548.187, 1550. 772 Å) with the proposed model. The green line indicates the difference between the observed and the
theoretical line profile.
In this figure we can see the fitting of the C IV UV doublet of an AGN (PG 0946+301) that presents DACs, with the proposed model.
In these figures we can see the fitting of some AGN spectral lines that present SACs, with the proposed model.
In these figures we can see the fitting of some AGN spectral lines that present SACs, with
the proposed model.
Conclusions1. Using the proposed model, we can calculate the values of some parameters such as the rotational, the random and the radial velocities, the FWHM, the optical depth, the absorbed or emitted Energy, the Column Density and the Gaussian Standard Deviation, as well as the relation among them. This means that now we can try to understand the mechanism that is responsible for the DACs or SACs phenomenon.2. The acceptance of SACs and DACs phenomena as the reason of the spectral lines complex structure lead us to accept smaller broadening, FWHM, optical depths, column densities and different rotation, radial and random velocities, because now the idea is that the complex line shape does non present a single spectral line, but a group of satellite components (DACs or SACs). From these new ideas we have taken different values of the parameters that, (perhaps) lead us to a different mechanism for the construction of the density regions that produce the DACs or SACs regions.
3. The detected time scale variation of the parameters values in the C IV, N IV, N V and Si IV density regions in the UV spectrum of the Oe star HD 93521 indicates that the radial, rotational and random velocities, the column densities, and the optical depths present only small variations.This fact lead us to accept that matter which creates DACs or SACs remains practically stable during the studied period of 18 years.An other explanation of this phenomenon is that in the area where we can detect high density regions, matter flows, and only the physical properties (conditions) which lead to high density, remain stable (for example magnetic fields or shocks from a companion in the case of a binary system).
But the main questions remain………
1.What is the origin and the mechanism that permit the periodic ejection of mass from the equator of rapidly rotating Hot Emission Stars?
2.What is the origin and the mechanism responsible for the construction and the long time stability of density regions that produce DACs and SACs phenomena and lie in the ejected matter?
These great questions and many others that arise from the study of hot emission stars and AGNs with the proposed model, wait for future answers.
Thank you very much for your attention