# Understanding the nature of the intriguing source X Persei: A deep look with a Suzaku observation

Chandreyee Maitra, Harsha Raichur, Pragati Pradhan, Biswajit Paul

<figure><img src="image_1.png" /></figure>

## To cite this version:

Chandreyee Maitra, Harsha Raichur, Pragati Pradhan, Biswajit Paul. Understanding the nature of the intriguing source X Persei: A deep look with a Suzaku observation. Monthly Notices of the Royal Astronomical Society, 2017, 470 (1), pp.713-722. 10.1093/mnras/stx1281. hal-01555094

HAL Id: hal-01555094

https://hal.science/hal-01555094v1

Submitted on 25 Aug 2025

HAL is a multi-disciplinary open access archive for the deposit and dissemination of scientific research documents, whether they are published or not. The documents may come from teaching and research institutions in France or abroad, or from public or private research centers.

L'archive ouverte pluridisciplinaire HAL, est destinée au dépôt et à la diffusion de documents scientifiques de niveau recherche, publiés ou non, émanant des établissements d'enseignement et de recherche français ou étrangers, des laboratoires publics ou privés.

<figure><img src="image_2.png" /></figure>
<figure><img src="image_3.png" /></figure>

# Understanding the nature of the intriguing source X Persei: a deep look with a *Suzaku* observation

Chandreyee Maitra,<fnref n="1" />*† Harsha Raichur,<fnref n="2" /> Pragati Pradhan<fnref n="3" /> and Biswajit Paul<fnref n="4" />

Accepted 2017 May 19. Received 2017 May 17; in original form 2016 October 18

## ABSTRACT

We present detailed broad-band timing and spectral analysis of the persistent, low luminosity and slowly spinning pulsar X Persei using a deep *Suzaku* observation of the source. The spectrum is unusually hard with a cyclotron resonance scattering feature (CRSF), the presence of which has been debated. By comparing the spectral models relevant for accretion-powered pulsars, we have obtained the best constraint on the broad-band spectral model of X Persei obtained so far. The CRSF is not confirmed in the average spectrum. We have also identified the presence of different intensity levels in the source with distinct changes in the pulse profile and the energy spectrum indicating changes in the accretion geometry. We further find evidence of a CRSF in the highest intensity levels at ~40 keV, indicating a magnetic field strength of $3.4 \times 10^{12}$ G.

**Key words:** stars: neutron – X-rays: binaries – X-rays: individual: X Persei.

## 1 INTRODUCTION

X Persei (4U 0352 + 309) is a binary stellar system at a distance of ~0.95 kpc (Telting et al. 1998) and consists of a slowly spinning neutron star (White, Mason & Sanford 1977, $P_{spin} \sim 837$ s) that is accreting matter from its Be-star companion (Lyubimkov et al. 1997). The source is peculiar in that it is a persistent source and does not show Type-I outbursts as are commonly observed in other Be-/X-ray binaries. But X-ray flares and variability in the X-ray light curve of the source have been observed (La Palombara & Mereghetti 2007; Lutovinov, Tsygankov & Chernyakova 2012). The orbital period of the binary system is long, $P_{orb} \sim 250$ d, but the orbital eccentricity is only $e \sim 0.11$ (Delgado-Martí et al. 2001). The long orbital period and the low X-ray luminosity of the source support the assumption that the neutron star in this binary is accreting quasi-spherically by capturing matter from the stellar wind of the Be-star (Shakura et al. 2012). The X-ray spectrum of X Persei is also unlike most accreting X-ray pulsars, the latter can usually be modelled with a power law and a cutoff in the range 10–30 keV (White, Swank & Holt 1983). Instead, X Persei has a peculiarly hard X-ray spectrum, making the source detectable at energies higher than 100 keV (Lutovinov et al. 2012). Thus, a single-component spectral model is insufficient to

model the source continuum spectrum, making it necessary to include a second high-energy component to explain the emission at harder X-rays. Several authors have used several different models to explain the observed spectrum, of which we note the following works. The *RXTE* observations were modelled using a blackbody component at lower energies and a power-law component with an exponential cutoff at higher energies (Coburn et al. 2001). A cyclotron resonance scattering feature (CRSF) was also required to account for an absorption-like feature seen around 30 keV. The spectrum obtained from *BeppoSAX* observation was modelled with two power-law components with exponential cutoffs at low and high energies and did not require any CRSF (Di Salvo et al. 1998). The *INTEGRAL* observations used thermal Comptonization and bulk motion Comptonization to account for the observed spectrum at the low and high energies, respectively (Doroshenko et al. 2012). The *INTEGRAL* observations also did not require any CRSF to improve the spectral model. Thus, the presence of CRSF noted in the *RXTE* observations was not detected in either the *BeppoSAX* or the *INTEGRAL* observation and hence needs to be verified. There is also no clear agreement on the unusual nature of the X-ray spectrum with respect to the continuum model.

## 2 OBSERVATION AND DATA REDUCTION

X Persei was observed using *Suzaku* in 2012 for a long duration of 153 ks. We present here the analysis of this observation. *Suzaku* is a broad-band X-ray observatory covering an energy range of

<footnote n="1">¹Laboratoire AIM, IRFU/Service d'Astrophysique – CEA/DSM – CNRS – Université Paris Diderot, Bat. 709, CEA-Saclay, F-91191 Gif-sur-Yvette Cedex, France</footnote>

<footnote n="2">²Nordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden</footnote>

<footnote n="3">³St Joseph's College, Singamari, Darjeeling 734104, West Bengal, India; North Bengal University, Raja Rammohanpur, Darjeeling 734013, West Bengal, India</footnote>

<footnote n="4">⁴Raman Research Institute, C.V. Raman Avenue, Sadashivanagar, Bangalore 560064, India</footnote>

<footnote>* E-mail: cmaitra@mpe.mpg.de</footnote>

<footnote>† Present address: Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany.</footnote>
<figure><img src="image_4.png" /><figcaption>**Figure 1.** Left figure shows the light curves in low- and high-energy bands with the lowest panel showing the HR. The light curves are binned at the spin period of 835.29 s. Right figure shows the HR plotted against the PIN count rate to highlight the variation in HR with the count rate in the high-energy band.</figcaption></figure>

0.2–600 keV (Mitsuda et al. 2007). The two main instruments on-board are (i) the X-ray Imaging Spectrometer (XIS: covering 0.2–12 keV) (ii) the Hard X-ray Detector (HXD: PIN diodes covering the range of 10–70 keV and GSO crystal scintillators detectors covering 70–600 keV). Therefore, the observation covers a wide energy band simultaneously and with high sensitivity making it possible to do detailed spectroscopic studies of the source.

The data were reduced and processed with the standard proce-
dures and using the latest CALDB version '20140825'. The XIS was
operated in the standard data mode with the 1/4 window mode that
provided a timing resolution of 2 s. The nominal pointing was set
to XIS. The XIS data was examined for the presence of pile-up. A
central region corresponding to a pile-up fraction >4 per cent was
discarded from all further analysis.

3 TIMING ANALYSIS: PULSATION SEARCH
AND LIGHT CURVES

We applied barycentric corrections to the event files for the timing
analysis, using the FTOOLS task 'aebarycen'. Orbital correction
was not required as the observation duration is much less than
the decoherence time-scale due to the orbital motion of the system
(Chakrabarty et al. 1997, decoherence time-scale is ~54 d, equation
A9). Light curves were extracted with a time resolution of 2 s
and 1 s, respectively, from the XISs (0.2–12 keV) and HXD/PIN
(10–70 keV). To search for pulsations in the data, pulse folding and
χ<fnref n="2" /> maximization technique was applied. Pulsations were found in
the light curve at 835.29 ± 0.29 s, which was subsequently used to
bin the light curves and also to create corresponding pulse profiles.

Fig. 1 shows the light curves in the low (XIS: 0.2–12 keV) and
high (PIN: 10–70 keV) energy bands along with the hardness ratio
(HR) curve, all binned at the spin period of the source. The ‘HR’
is defined as the ratio of the count rate in the XIS band (with
the three XISs added together) to the PIN band. It is clear from
the figure that the count rates in both the energy bands vary by
a factor up to 5 during the observation. Moreover the HR shows
a variation by a similar factor with the PIN count rate (see right
of Fig. 1) that indicates spectral variability in the source. In order
to investigate the true energy dependence of the pulse profiles in
this source and to construct an average model of the representative
X-ray spectrum of the source, it is important to choose a time
interval free from intensity or spectral variations. Therefore, in order
to construct the pulse profiles and the energy spectrum of X Persei,

we choose a stretch of the observation where 0.02 < HR < 0.03
and 0.8 < PINc/s < 1.4, as not much spectral variation is expected
in this narrow stretch.

**3.1 Energy dependence of the pulse profiles**

To investigate any possible energy dependence of the pulse profiles,
we created the energy resolved pulse profiles by folding the data in
different energy bands at the obtained pulse period. We have only
used XIS and PIN light curves for the purpose between the energy
ranges 0.5–12 and 10–70 keV, respectively. Pulsations are detected
up to 100 keV asserting the hard nature of the source as seen from the
pulse profile created using the GSO light curve. Energy-dependent
pulse profiles are shown in Fig. 2. The pulse profiles are more or
less sinusoidal in shape from 0.5 to 100 keV with little evolution
with energy. This is consistent with previous results from the *RXTE*
and *BeppoSAX* observations (Di Salvo et al. 1998; Coburn et al.
2001). An additional spike-like feature is evident at phase ~0.4
in the low-energy pulse profiles (≤12 keV) that do not show any
evolution of its strength with energy in these energy bands. The
high-energy pulse profiles are featureless.

4 SPECTRAL ANALYSIS

Spectral analysis was performed using *XSPEC* v12.8.1.<fnref n="1" /> The XIS
spectra were fitted from 0.8 to 10 keV and the PIN spectrum from
10 to 70 keV and GSO between 50 and 110 keV. The energy range
of 1.75–2.23 keV was neglected due to artificial structures in the
XIS spectra around the Si edge and Au edge. For the XIS spectrum,
we grouped the energy ranges between 0.8–6 and 6–7 keV by 8,
4 and the rest by a factor of 8, respectively. This ensured that we
had enough counts in each channel to apply χ<fnref n="2" /> statistics for fitting
the spectra. The energy around Fe line (6–7 keV) was binned by a
smaller factor to avoid losing information on a narrow line feature,
if any. The whole energy range of the PIN spectrum was binned
by a factor of 4, for the reason mentioned above. For binning the
GSO spectrum, we used the suggested grouping method for GSO
spectrum with ‘gsobgd64bins.dat’ available in the *Suzaku* analysis
homepage.<fnref n="2" />

<footnote n="1">¹ https://heasarc.gsfc.nasa.gov/xanadu/xspec/</footnote>

<footnote n="2">² http://heasarc.gsfc.nasa.gov/docs/suzaku/analysis/abc/</footnote>
<figure><img src="image_5.png" /><figcaption>**Figure 2.** Energy-resolved pulse profiles of X Persei from XIS (left), PIN (right) and GSO data (last figure in the right-hand panel). The energy ranges are marked inside the panels.</figcaption></figure>

**4.1 Broad-band spectroscopy and the average energy spectrum**

The spectra of accretion-powered pulsars are usually modelled phenomenologically using a power law with quasi-exponential high-energy cutoff of various functional forms. The most widely used models are a power law with a high-energy exponential cutoff, a broken power law (White, Swank & Holt 1983; Mihara 1995; Coburn 2001) or a Fermi–Dirac cutoff (Tanaka 1986, XSPEC model ‘fdcut’). More recently, a smoothed high-energy cut-off model (XSPEC model ‘newhcut’) is also used extensively as it avoids artificial residuals in the spectra due to the abrupt nature of the exponential cut-off model. Other models are a combination of two power laws with different photon indices but common cut-off energy value called the negative and positive power laws with exponential model (Mihara 1995; Makishima et al. 1999, XPEC model ‘NPEX’), and a thermal Comptonization model (XPEC model ‘CompTT model’). Recently, a new model for X-ray continuum formation has been developed for accretion-powered pulsars with high magnetic fields ($B \ge 10^{12}$ G) assuming a cylindrical geometry and a constant B permeating it. In this model, the source of seed photons is assumed to be from the blackbody photons arising from the base of the accretion column. This model was also successfully applied to the spectra of Supergiant Fast X-ray Transients that are relatively low-luminosity sources ($L_x \le 10^{34}$ erg s⁻¹), and is available as a standard XPEC model ‘COMPMAG’ (Farinelli et al. 2012). The model allows fitting parameters related to the physics of accretion on to a high magnetic field neutron star, for example η (index of the velocity profile), β (terminal velocity of the accreting matter at the neutron star surface) and $r_0$ (radiation of the accretion column in terms of Schwarzchild radius), in addition to the electron temperature and optical depth of the accreting column and the temperature of the seed blackbody photon. An updated version of this model (XPEC model ‘COMPMAG2’) has also been developed by the authors that also

considers the contribution of bremsstrahlung and cyclotron emission as the source of seed photons for Comptonization (Farinelli et al. 2016). This effect is more relevant for high-luminosity X-ray pulsars where the contribution of Comptonized blackbody has been found to be negligible with respect to the Comptonized bremsstrahlung and cyclotron emission. The model also has many additional parameters compared to ‘COMPMAG’, for example the height of the accretion column in addition to its radius, and the magnetic field strength B of the neutron star surface. Additionally, it provides options to choose the source of seed blackbody photons, as well as the beam pattern between pencil and fan.

We tried to fit the broad-band energy spectrum of X Persei with all the different continuum models mentioned above. The spectrum extends up to 100 keV and as in the previous works using the BeppoSAX (Di Salvo et al. 1998), RXTE (Coburn et al. 2001) and INTEGRAL (Doroshenko et al. 2012) observations, a two-component model is required to fit separately the low- and the high-energy part of the broad-band Suzaku spectrum (using XIS+PIN+GSO). Spectra obtained from XIS, PIN and GSO instruments were fitted simultaneously allowing for cross-calibration constants for the PIN and GSO instruments with respect to the XIS instrument. In all the cases, we applied a Galactic line-of-sight absorption (XPEC model ‘tbabs’) component to the continuum models. No Fe line was detected in the spectrum. A broad emission feature at 1.65 keV was however detected only in the XIS1 (BI CCD) spectrum. As this was detected only in one of the three XISs, this may be an instrumental feature and was hence not included in the analysis.

For all the phenomenological continuum models, a broad absorption feature (~30 keV) was evident in the residuals, reminiscent of the CRSF reported from the RXTE observations. Adding CRSF absorption profile (‘cyclabs’ in XPEC) to the spectrum improved the fit. Another point we noted is that since the spectrum of X Persei is unusually hard and extended >100 keV, the GSO spectrum was crucial to constrain the cutoff in the high-energy range, as it mostly
appeared to be a hard tail-like feature in the PIN band (10–70 keV). Overall, we found a two-component power-law model with smooth exponential rollover (model ‘newhcut’) as the best representative phenomenological continuum model of the X-ray spectrum of X Persei, since it provided the best-fitting quality with respect to the reduced $\chi^2$ (1.70 for 567 dof). The corresponding decrease in $\chi^2$ after the inclusion of the CRSF was 11. However, the observed feature was shallow and broad, with a width of ~12 keV. This is broader than most of the CRSFs observed, and a broad absorption feature as this could artificially modify the continuum spectrum considerably. Therefore, it could arise from an artefact due to inadequate modelling of the continuum emission, and should be treated with caution. The best-fitting continuum parameters obtained using the ‘newhcut’ model are consistent with the results obtained using BeppoSAX observation. However, *Suzaku* being more sensitive than the former in the high-energy range, the high-energy parameters are better constrained.

Thereafter, we proceeded to fit the broad-band spectrum with the analytical model ‘COMPMAG’ and its updated version. The ‘COMPMAG’ model has many spectral parameters that were impossible to constrain simultaneously. Especially, $\beta$ if left free preferred a value >0.9 in the fit, which is greater than the maximum possible terminal velocity at the neutron star surface. Therefore, we tested the two-component ‘COMPMAG’ model, assuming reasonable parameter values applicable to low-luminosity accretion-powered pulsars, i.e. free-fall velocity profile ($\eta = 0.5$), and $\beta = 0.5$ that corresponds to the maximum terminal velocity at the neutron star surface, and a pencil beam emission pattern. The radius of the accretion column ($r_0$) was set to 0.25 corresponding to a radius of ~1 km for a neutron star of mass 1.4 $M_\odot$. The Albedo at the neutron star surface (A) was set to 1. This provided an acceptable fit to the data with acceptable and physically viable parameter values. Addition of a CRSF feature was not required for this model. The high $\beta$ preferred by the fit indicated that bulk motion Comptonization (BMC) dominates the Comptonization process in X Persei. The fit also provided a low value of electron temperature ($kT$) consistent with the high value of $\beta$ obtained (Farinelli et al. 2012). The dominance of BMC in low-luminosity pulsars, especially X-Persei has been predicted before and is consistent with our results (Becker & Wolff 2005, 2007). In Becker & Wolff (2007), the authors qualitatively described the observed spectrum of X-Persei with a pure BMC model. The obtained reduced $\chi^2$ value with ‘COMPMAG’ was higher than that obtained with the ‘newhcut’ model (1.84 for 569 dof), although there were no systematic pattern in the residuals, and the higher $\chi^2$ was mainly contributed by a higher variance in a few energy bins of the XIS spectra. Fit with the updated ‘COMPMAG2’ model was difficult with the given statistical quality of the data, as it required fitting many more additional parameters. Moreover as discussed in Farinelli et al. (2016), the ‘COMPMAG’ model provides an adequate description of the spectrum for low-luminosity pulsars, where the blackbody emission provides the major source of photons for Comptonization, appropriate for the case of X Persei. Considering the above, and as ‘COMPMAG’ is a more physical model to understand the continuum spectra of the source, we used this as our best-fitting model for the rest of the paper. As a CRSF feature is not required for this model, we cannot claim the presence of a CRSF in the average spectrum of X Persei. Table 1 summarizes the best-fitting broad-band spectral parameters obtained using the ‘newhcut’ (without addition of the CRSF) and ‘COMPMAG’ models. Fig. 3 shows the best-fitting unfolded spectrum for the best-fitting model, showing the model components.

<table><caption>**Table 1.** Best-fitting phase-averaged spectral parameters of X Persei. Errors quoted are for 90 per cent confidence range.</caption><thead><tr><th>Parameters</th><th>newhcut</th><th>COMPMAG</th></tr></thead><tbody><tr><td>N<sub>H</sub> (10<sup>22</sup> atoms cm<sup>-2</sup>)</td><td>0.39 ± 0.003</td><td>0.17 ± 0.005</td></tr><tr><td>Γ<sub>1</sub> (low energy)</td><td>0.28 ± 0.01</td><td>—</td></tr><tr><td>E1-folding energy (keV)</td><td>3.49 ± 0.03</td><td>—</td></tr><tr><td>E1-cut energy (keV)</td><td>2.98 ± 0.03</td><td>—</td></tr><tr><td>Γ<sub>2</sub> (high energy)</td><td>1.52 ± 0.03</td><td>—</td></tr><tr><td>E2-cut energy (keV)</td><td>56.26 ± 10</td><td>—</td></tr><tr><td>KT<sub>bb</sub> (keV)</td><td>—</td><td>0.86 ± 0.03</td></tr><tr><td>kT<sub>1</sub> (keV)</td><td>—</td><td>0.21 ± 0.02</td></tr><tr><td>τ<sub>1</sub></td><td>—</td><td>0.12 ± 0.02</td></tr><tr><td>kT<sub>2</sub> (keV)</td><td>—</td><td>2.3 ± 1.2</td></tr><tr><td>τ<sub>2</sub></td><td>—</td><td>6.3 ± 0.5</td></tr><tr><td>Flux (XIS)<sup>a</sup> (0.3–10 keV)</td><td>6.62 × 10<sup>-10</sup> ± 0.41</td><td>6.75 × 10<sup>-10</sup> ± 0.43</td></tr><tr><td>Flux (PIN)<sup>a</sup> (10–70 keV)</td><td>7.43 × 10<sup>-10</sup> ± 0.11</td><td>7.40 × 10<sup>-10</sup> ± 0.12</td></tr><tr><td>L<sub>x</sub><sup>b</sup> (0.3–70 keV)</td><td>1.6 × 10<sup>35</sup></td><td>1.6 × 10<sup>35</sup></td></tr><tr><td>reduced χ<sup>2</sup>/d.o.f</td><td>1.73/569</td><td>1.83/569</td></tr></tbody></table>

Notes. $^a$Observed flux in units of erg cm$^{-2}$ s$^{-1}$ in the mentioned energy band.

$^b$Bolometric unabsorbed luminosity in units of erg s$^{-1}$ in the mentioned energy band, assuming a distance of 1 kpc.

<figure><img src="image_6.png" /><figcaption>**Figure 3.** The upper panel shows the unfolded best-fitting average (or representative) energy spectrum of X Persei showing the different continuum model components; the bottom panel shows the residues of the best-fitting model.</figcaption></figure>

## 5 INTENSITY LEVELS

The light curves of X Persei in both the low- and high-energy bands show variations in the count rate up to a factor of 5. As mentioned earlier, large variation in the ‘HR’ is also observed (see Fig. 1). This motivated us to search for different intensity levels in the observation. This was done using the combined XIS light curve. For this, the light curve was first binned using the determined spin period of the source. Then, we plotted the number of bins as a function of the count rate to get a histogram that is shown in Fig. 4. From the histogram, we identified the ‘High’ and ‘Low’ levels from the two ends of the distribution, or the tail regions. The intermediate level was identified from the peak of the distribution. Fig. 4 also hinted a double-peaked feature of the distribution. Hence, we subdivided the intermediate level into ‘Intermediate1’ (Int-1 from now) and ‘Intermediate2’ (Int-2 from now) levels.

The intensity levels chosen for this work are also shown in the figure, and the details are tabulated in Table 2.
<figure><img src="image_7.png" /><figcaption>**Figure 4.** Figure shows the histogram of the combined light curve of X Persei as observed by the *Suzaku* XIS detectors. Count rates demarking different intensity levels used in the subsequent analysis are shown with vertical lines.</figcaption></figure>

<table><caption>**Table 2.** Table detailing the different intensity levels chosen for this work.</caption><thead><tr><td>Intensity level</td><td>Count rate (c s<sup>-1</sup>)</td><td>Exposure (ks)</td></tr></thead><tbody><tr><td>Low</td><td>&lt;31</td><td>11.4</td></tr><tr><td>Int-1</td><td>≥31 and ≤45</td><td>54.2</td></tr><tr><td>Int-2</td><td>≥45 and ≤65</td><td>65</td></tr><tr><td>High</td><td>&gt;65</td><td>10.5</td></tr></tbody></table>

To investigate whether these are distinct intensity levels associated with changes in the accretion geometry we investigated the pulse profiles and the broad-band spectrum of the source at different intensities. The results are presented in the subsequent subsections. Changes in the pulse profiles and the energy spectrum with intensity is associated with corresponding changes in the conditions of the accretion column (Becker et al. 2012).

## 5.1 Intensity dependence of pulse profiles

Fig. 5 shows the normalized background subtracted pulse profiles of X Persei at different intensity levels extracted from XIS (0.5–10 keV), PIN (10–70 keV) and GSO (50–100 keV) light curves, respectively. The pulse profiles exhibit noticeable evolution with intensity at all energy ranges. For the entire energy band, the profiles become narrower as the intensity increases. The shoulder-like feature between phase range 0.1–0.3 seen at the ‘Low’ and ‘Int-1’ state gradually morphs to a sharp narrow profile. Another important feature is that the corresponding pulse fraction increases. In the XIS energy band, the pulse fraction increases from 44 per cent to 68 per cent between the ‘Low’ and ‘High’ intensity levels, while the corresponding numbers in the PIN energy band are 47 per cent and 67 per cent. It may be mentioned that La Palombara & Mereghetti (2007) reported an increase in pulse fraction with intensity from the RXTE-PCA data. Changes in the pulse profiles with intensity have been reported before in several accretion-powered pulsars like Her X-1 (Klochkov et al. 2008), 4U 0115+63 (Tsygankov et al. 2007) and GX 304-1 (Malacaria et al. 2015). The changes can be qualitatively understood due to changes in the height and geometry of the accretion column with intensity. The results point towards a change in the accretion geometry and a gradual

evolution in the beaming pattern with increasing intensity with the highest intensity showing the highest beamed pulse profile. Detailed modelling of the shape of the pulse profiles with intensity requires an accurate description of the magnetic field geometry, scattering cross-sections as well as the energy and intensity dependence of the emission beam itself, and is beyond the scope of this work.

## 5.2 Intensity dependence of the energy spectrum

We extracted spectrum corresponding to the intensity levels mentioned in Section 5. We started the fits with the best-fitting model (obtained with ‘COMPMAg’) of the average spectrum to fit the spectra at different intensity levels. Like the pulse profiles, the energy spectrum also exhibits dependence with intensity. We noticed the presence of a very weak Fe Kα emission line (equivalent width $7.5 \pm 2.1$ eV), in the ‘Int-1’ intensity state. This might be because at this intensity level, the continuum emission is suppressed, and yet the statistical quality of the spectrum is enough to detect the line. The electron temperature ($kT2$) of the ‘High’ intensity level is higher than in other spectra, indicating a harder spectrum consistent with the highest pulse fraction of the corresponding hard X-ray pulse profile (see Fig. 5). A correlation between the HR and intensity, with indication of increasing hardness with intensity has been reported previously in the XMM–Newton band <15 keV (La Palombara & Mereghetti 2007). The harder spectrum at ‘High’ intensity may indicate an increase in Comptonization in the accretion column. The parameter $kT2$ however only traces the thermal Comptonization component. The change in the BMC component, thought to be dominant in X Persei cannot be probed. This is because $\beta$ cannot be left free in the fits, due to statistical limitations. The errors bar of the parameter $kT2$ is however high due to the low exposure time of the spectrum, and therefore the increase in $kT2$ in not statistically significant. The other continuum parameters do not show noticeable evolution with intensity.

The most significant changes are dip-like features present in the spectrum of the ‘High’ and ‘Int-2’ intensities at ~40 keV, reminiscent of a CRSF. Both the residuals and the corresponding $\chi^2$ improved after addition of a CRSF feature (‘cyclabs’ model in XPEC). For the ‘Int-2’ spectrum, additional residuals, reminiscent of another feature was noticed at ~29 keV. Adding another CRSF improved the $\chi^2$ further. The width of this feature could not be constrained and was hence frozen at 3 keV. The total improvement in $\chi^2$ for the ‘High’ and ‘Int-2’ intensity levels was 20 and 18 after adding the CRSF (1 for ‘High’ and 2 for ‘Int-2’) for 2 dof and 4 dof, respectively. In order to verify whether this was a model-independent feature, we checked the spectral fits for the intensity states, using the ‘newhc’ spectral model. Residuals are seen at the same energies for the ‘High’ and ‘Int-2’ spectra. However, the dips are much wider and deeper. As discussed in Section 4.1, this difference might arise due to insufficient continuum modelling of the continuum spectrum with the ‘newhc’ spectral model. To further verify the presence of the CRSF in a model-independent manner, we extracted the ratio of the spectrum of the ‘High’ and ‘Int-2’ levels, respectively, divided by the average spectrum. Fig. 6 shows the ratio plots, with the dip at ~40 keV clearly visible. A detailed discussion on statistical significance of the CRSF is included in the next section. Fig. 7 shows the unfolded spectrum of X Persei (showing the model components) at different intensity levels with and without inclusion of the CRSF feature for the ‘High’ and ‘Int-2’ intensities. The best-fitting parameters are tabulated in Table 3, including the CRSFs for intensity level ‘High’ and ‘Int-2’.
<figure><img src="image_8.png" /><figcaption>**Figure 5.** Normalized background subtracted pulse profiles of X Persei at different intensity levels constructed from XIS (0.5–10 keV) (left-hand panel), PIN (10–70 keV) (middle panel) and GSO (50–100 keV) (right-hand panel) light curves, respectively. Pulse profiles in Low, Int-1, Int-2 and High intensity levels are plotted in red, green, blue and black, respectively.</figcaption></figure>

<figure><img src="image_9.png" /><figcaption>**Figure 6.** Ratio plot of intensity levels ('High' and 'Int-2') to average spectra. The dip at ~40 keV is evident.</figcaption></figure>

## 5.3 CRSF and its detection significance

Computing statistical significance of CRSFs needs to be handled with care, as this is a multiplicative component modifying the underlying continuum itself. In order to assess whether the improvement in $\chi^2$ is significant, the standard F-test cannot be used which is suitable only for additive components (Protassov et al. 2002). Therefore, we used two independent tests to access the significance of CRSFs in the ‘High’ and ‘Int-2’ intensity spectra.

At first we performed a numerical evaluation of the significance of the CRSF by performing Monte Carlo simulations. This was done with the xpec script lrt by simulating large number of data sets (3001) with the two-component ‘COMPMAG’ model without the CRSF, modified with statistical (Poisson) noise. At each iteration, the simulated data sets were fitted with the continuum model with and without the CRSF and the statistics were compared. For the ‘High’ spectrum, we found that in 824 out of 3001 cases, the simulated $\chi^2$ was as high as the observed one. This gave a PCI of 27 per cent. In case of the ‘Int-2’ spectrum with a similar analysis, the obtained result was 34 per cent. Considering the high PCI values in both cases, the CRSF at ~40 keV cannot be considered statistically significant. Performing the simulation with two CRSFs instead of one, for the ‘Int-2’ spectrum gave

only slightly better results and cannot be considered statistically significant.

The evaluation of the statistical significance of a CRSF, which is often a weak absorption feature against the continuum is recommended to be supported by other tests, especially one that is sensitive to the structure of the residuals, in order to distinguish a random fluctuation from a systematic structure (Sguera et al. 2011; Orlandini et al. 2012). In the spectral fits of the ‘High’ and ‘Int-2’ spectra, the errors dominate as is evident from the best-fitting parameters in Table 3. Therefore, we performed a run-test (Barlow 1989) on the residuals between 30 and 50 keV (range in which CRSF is detected) for the ‘High’ spectrum, in order to test for the null hypothesis of the randomness of the residuals of the fit in that energy range. The number of data points ($N_t$) was 14, with 3 points above zero ($N_+$), and 11 below zero ($N_-$). This gave a probability of obtaining $N_r \le 3$ ($N_r$ is the number of runs) equals 0.009 (0.9 per cent). In the case of ‘Int-2’ spectrum in the same energy range, $N_t$ was 14, with 5 $N_+$, and 9 $N_-$, which resulted in probability of obtaining $N_r \le 3$ equals 0.003 (0.3 per cent). The obtained values strongly indicated that the residuals are not due to random fluctuations, and have a systematic structure, indicating the need to add the CRSF component to the spectra. For the ‘Int-2’ spectrum, we also performed the test between 25 and 41 keV, to look for the
<figure><img src="image_10.png" /><figcaption>**Figure 7.** Best-fit unfolded X-ray spectrum of X Persei at different intensity levels ('High'–top left; 'Int-2'–top right; 'Int-1'–bottom left, 'Int-1'–bottom right) constructed from XIS (0.5–10 keV), PIN (10–70 keV) and GSO (50–100 keV). The upper panel shows the best-fitting energy spectrum, and the bottom panel shows the residues of the best-fitting model without including the CRSF (for 'High' and 'Int-2' spectra).</figcaption></figure>

<table><caption>**Table 3.** Best-fitting spectral parameters of X Persei for different intensity levels. Errors quoted are for 90 per cent confidence range.</caption><thead><tr><th>Parameters</th><th>High</th><th>Int-2</th><th>Int-1</th><th>Low</th></tr></thead><tbody><tr><td>N<sub>H</sub> (10<sup>22</sup> atoms cm<sup>-2</sup>)</td><td>0.20 ± 0.008</td><td>0.20 ± 0.002</td><td>0.17 ± 0.005</td><td>0.14 ± 0.009</td></tr><tr><td>KT<sub>bb</sub> (keV)</td><td>0.95 ± 0.02</td><td>0.90 ± 0.01</td><td>0.86 ± 0.03</td><td>0.83 ± 0.05</td></tr><tr><td>kT1 (keV)</td><td>0.23 ± 0.10</td><td>0.22 ± 0.02</td><td>0.20 ± 0.05</td><td>0.20 ± 0.15</td></tr><tr><td>τ1</td><td>0.12 ± 0.03</td><td>0.11 ± 0.01</td><td>0.10 ± 0.02</td><td>0.10 ± 0.04</td></tr><tr><td>kT2 (keV)</td><td>2.8 ± 0.5</td><td>2.3 ± 0.2</td><td>2.3 ± 1.1</td><td>1.7<sup>+2.2</sup><sub>-0.5</sub></td></tr><tr><td>τ2</td><td>6.0 ± 0.2</td><td>6.0 ± 0.1</td><td>6.0 ± 0.4</td><td>7.0 ± 0.7</td></tr><tr><td>CRSF D</td><td>0.54 ± 0.15</td><td>0.22<sup>+0.13</sup><sub>-0.08</sub></td><td>—</td><td>—</td></tr><tr><td>CRSF E (keV)</td><td>37.8 ± 2.4</td><td>40.8 ± 2.0</td><td>—</td><td>—</td></tr><tr><td>CRSF W (keV)</td><td>5.8<sup>+2.0</sup><sub>-2.4</sub></td><td>3.7<sup>+5.2</sup><sub>-2.1</sub></td><td>—</td><td>—</td></tr><tr><td>CRSF D<sub>1</sub> (keV)</td><td>—</td><td>0.15 ± 0.08</td><td>—</td><td>—</td></tr><tr><td>CRSF E<sub>1</sub> (keV)</td><td>—</td><td>28.6 ± 1.5</td><td>—</td><td>—</td></tr><tr><td>CRSF W<sub>1</sub> (keV)</td><td>—</td><td>3 (fixed)</td><td>—</td><td>—</td></tr><tr><td>Fe Kα (keV)</td><td>—</td><td>—</td><td>6.40 ± 0.00</td><td>—</td></tr><tr><td>eqw (keV)</td><td>—</td><td>—</td><td>7.5 ± 2.0</td><td>—</td></tr><tr><td>Flux (XIS)<sup>a</sup> (0.3–10 keV)</td><td>11.97 × 10<sup>-10</sup> ± 0.03</td><td>9.18 × 10<sup>-10</sup> ± 0.02</td><td>9.76 × 10<sup>-10</sup> ± 0.01</td><td>4.91 × 10<sup>-10</sup> ± 0.02</td></tr><tr><td>Flux (PIN)<sup>a</sup> (10–70 keV)</td><td>14.12 × 10<sup>-10</sup> ± 0.91</td><td>10.73 × 10<sup>-10</sup> ± 0.24</td><td>8.32 × 10<sup>-10</sup> ± 0.71</td><td>3.69 × 10<sup>-10</sup> ± 0.65</td></tr><tr><td>L<sub>x</sub><sup>b</sup> (0.3–70 keV)</td><td>3.0 × 10<sup>35</sup></td><td>2.3 × 10<sup>35</sup></td><td>1.6 × 10<sup>35</sup></td><td>1.4 × 10<sup>35</sup></td></tr><tr><td>reduced χ<sup>2</sup>/d.o.f (no CRSF)</td><td>—</td><td>—</td><td>1.87/557</td><td>1.21/555</td></tr><tr><td>reduced χ<sup>2</sup>/d.o.f (1 CRSF)</td><td>1.35/573</td><td>—</td><td>—</td><td>—</td></tr><tr><td>reduced χ<sup>2</sup>/d.o.f (2 CRSFs)</td><td>—</td><td>1.95/554</td><td>—</td><td>—</td></tr></tbody></table>

Notes. <sup>a</sup>Observed flux in units of erg cm<sup>-2</sup> s<sup>-1</sup>.

<sup>b</sup>Bolometric unabsorbed luminosity in units of erg s<sup>-1</sup> in the mentioned energy band, assuming a distance of 1 kpc.

additional absorption feature at 29 keV. In this case, $N_t$ was 11, with 3 $N_+$, and 8 $N_-$ This gave a probability of obtaining $N_r$ ≤ 3 equals 0.01 or a 1 per cent probability of the structure being due to random fluctuations. The low values obtained in all three cases

provide statistical evidence that the residual patterns are not due to random fluctuations.

Although the detection of the CRSF in the high-intensity levels of X Persei is not very statistically significant in terms of the delta $\chi^2$
and the comparison of the $\chi^2$ statistics with and without inclusion of the CRSF in the spectral model, there is strong indication that the feature is indeed present in the spectrum. This is supported from the results of the run-test and the model independent verification of the feature. Future deep observations will ascertain this further.

# 6 DISCUSSION

We have performed a comprehensive analysis of X Persei using a long Suzaku observation where we have probed several timing and spectral aspects of the source in detail. The broad-band sensitive instruments onboard Suzaku have allowed us to model the continuum spectra robustly and make comparison amongst several spectral models. We have found a two-component model suitable for the hard X-ray spectrum extending up to 100 keV as in previous works. There is also strong evidence that BMC dominates the Comptonization process as expected for low-luminosity accretion-powered pulsars with a hard continuum spectrum. The most intriguing aspect of this work is that we have identified for the first time, associated with changes in the pulse profile, corresponding indications of changes in the continuum spectra with varying intensity levels, pointing to changes in the accretion geometry. We have also found evidence of a CRSF at ~40 keV at the highest intensity levels, reinstating the magnetic field strength of the neutron star.

## 6.1 Broadband continuum modelling

Several previous works have attempted to model the energy spectrum of X Persei, the most notable being Di Salvo et al. (1998) (using BeppoSAX observation), Coburn et al. (2001) (using RXTE observation) and more recently Doroshenko et al. (2012) (using INTEGRAL observation). However, these results were based on instruments that were sensitive over different energy ranges and were unable to constrain either the low-energy part of the spectrum (in the case of RXTE and INTEGRAL) or the high-energy part (in the case of BeppoSAX) well. X Persei being a low-luminosity source with the energy spectrum ranging below 1 keV to above 100 keV, the instruments onboard Suzaku were ideal in this regard. We have tested all the continuum models presently available to fit the broad-band spectrum of accretion-powered pulsars. In all the cases, we required a two-component model separately for the low- and high-energy part of the spectrum as has also been reported in previous works. We find that a power-law component with a smooth exponential rollover provides the best fit both in terms of reduced $\chi^2$ and realistic values for the continuum parameters. The continuum model parameters we obtain are consistent with Di Salvo et al. (1998) who use the same model to describe the BeppoSAX spectrum. Our results are also consistent with Coburn et al. (2001) who use a blackbody component to model the low-energy part and a power-law component with an exponential rollover for the high-energy ranges of the spectrum. This is because while the parameters of the hard power-law component are similar, we note that RXTE-PCA being sensitive only >3 keV cannot differentiate between a 1.7 keV blackbody component (that they obtained) from a $\Gamma \sim 0.3$ power law having a rollover at ~3.5 keV (this work). The fit with the 'newcut' continuum model however indicated a broad absorption feature at ~30 keV in the residuals that can be identified with the CRSF previously reported in the source. Spectral fit with the analytical model 'COMPMAG' also provides an acceptable fit, and allows constraining physical parameters related to the accretion on the pulsar. The absorption feature at 30 keV is not required

by this model indicating that it might be an effect due to insufficient continuum modelling with the phenomenological models, and needs to be treated with caution.

The spectral fit with 'COMPMAG' model fitted with simple assumptions suitable for low-luminosity accreting pulsars provides a direct insight into the process of spectral formation, and the conditions of the accretion column. The best-fitting average spectrum indicated a high value of $\beta$ indicating that BMC dominates the Comptonization process in X Persei.

The broad-band unabsorbed bolometric luminosity of X Persei (0.3–70 keV) is $L_x = 1.6 \times 10^{35}$ erg s$^{-1}$. In accretion-powered pulsars with luminosity $L_x < 10^{37}$ erg s$^{-1}$, it is widely believed that the radiation is mainly generated from the hotspots generated by the infalling plasma that decelerates to the surface of the neutron star due to Coulomb interactions forming an accretion mound (Burnard, Arons & Klein 1991). In such sources, BMC is believed to play an important role. Further, this model has been particularly preferred to fit the spectrum of steep sources like X Persei (Becker & Wolff 2007, 2005). This is in agreement with our obtained results. The hard power-law tail in the PIN energy range with a rollover at energies much higher than expected for accreting pulsars (~56 keV), is in further support of this.

## 6.2 Intensity levels

We report the presence of large flux variations in the observation and divided the duration into four different intensity levels: (a) High, (b) Intensity 2, (c) Intensity 1 and (d) Low ordered by decreasing count rates where the difference between the highest and the lowest intensity levels is a factor of ~5. To investigate whether there are distinct timing and spectral characteristics of the source at different intensity levels, we extracted pulse profiles in the low- and high-energy band as well as the broad-band spectrum corresponding to these intensity levels. We confirm that there are indeed associated changes in the pulse profile, the corresponding spectrum, with the source flux. For all the energy ranges, we see that the pulse profiles become narrower with increasing intensity with an increase in pulse fraction from 44 per cent to 68 per cent at the highest intensity level. There is also an indication that the highest intensity level ('High') has a harder spectrum. The highest intensity levels ('High' and 'Int-2') also indicate the presence of a CRSF at ~40 keV. The changes in the pulse profile and the energy spectrum reflects a change in the beam function and a change in the conditions of the accretion column with intensity.

In accretion-powered X-ray pulsars, the 'critical luminosity' $L_{crit}$ divides two regimes of accretion into the super and sub-critical regime (Becker et al. 2012). The equation is given by

$$L_{\text{crit}} = 1.49 \times 10^{37} \text{ erg s}^{-1} \left(\frac{\Lambda}{0.1}\right)^{-7/5} w^{-28/15} \\ \times \left(\frac{M}{1.4 \text{ M}_\odot}\right)^{29/30} \left(\frac{R}{10 \text{ km}}\right)^{1/10} \left(\frac{B_{\text{surf}}}{10^{12} \text{ G}}\right)^{16/15} \quad (1)$$

Here, R, M and B are the radius, mass and surface magnetic field strength (B in terms of $\sim 10^{12}$ G) of the neutron star. The parameter $\Lambda = 0.1$ approximates the case of disc accretion, and $\Lambda = 1.0$ is suitable for wind accretors, although it is difficult to determine the parameter precisely for an assumption of spherical accretion. $w = 1$ on the other hand, characterizes the shape of the photon spectrum inside the column (where there is assumed to be a mean photon energy of $\bar{E} = w k T_{\text{eff}}$), and $\Lambda$ characterizes the mode of accretion. For X Persei, it is reasonable to assume the value of $\Lambda$ for wind
<table><caption>**Table 4.** Table comparing measured flux of X Persei using different instruments.</caption><thead><tr><th>Instrument</th><th>Flux<br>1–10 keV</th><th>CRSF detected<br>–</th></tr></thead><tbody><tr><td><i>BeppoSAX</i></td><td>1.7</td><td>NO</td></tr><tr><td><i>RXTE</i></td><td>2.1</td><td>YES</td></tr><tr><td><i>INTEGRAL</i></td><td>1.9</td><td>NO</td></tr><tr><td><i>Suzaku</i> (average)</td><td>6.6</td><td>NO</td></tr><tr><td><i>Suzaku</i> ('Int-2' intensity)</td><td>9.0</td><td>YES</td></tr><tr><td><i>Suzaku</i> ('High' intensity)</td><td>11.7</td><td>YES</td></tr></tbody></table>

Notes. <sup>a</sup>Flux is in units of $10^{-10}$ erg cm$^{-2}$ s$^{-1}$.

accretors i.e. 1. Therefore, we obtain $L_{crit} = 2.1 \times 10^{36}$ erg s$^{-1}$ assuming $B = 3.4 \times 10^{12}$ G (obtained from the CRSF centroid energy of ~40 keV), and standard values for the mass and radius of the neutron star. This is above the bolometric luminosity of $1.4 \times 10^{35}$ erg s$^{-1}$ of the source, which indicates the source is in the sub-critical regime with the emission dominating from the accretion mound. In this regime, the characteristic emission height, from where most of the radiation escapes, decreases with increasing luminosity. So, at a higher intensity if the accretion mound is pressed closer to the neutron star surface owing to a higher ram pressure of the infalling material, one might be probing the hotter base of the accretion mound with a higher fraction of higher energy photons generated due to Comptonization, which gives rise to a harder and more beamed emission. Our results are also consistent with Postnov et al. (2015) that investigated the behaviour of the spectral HR as a function of X-ray luminosity in a sample of X-ray pulsars at an energy range <12 keV (using the *RXTE-ASM* data). The authors observed an increase in HR with increasing luminosity for sources in the sub-critical regime. The increasing hardness with luminosity in X Persei are observed at energies $\le 110$ keV (the upper limit for the spectral fitting band), and indicates that the postulate is also valid in a broad energy band.

## 6.3 Cyclotron line

A very interesting outcome of this work is the indication of the presence of the CRSF at the high-intensity levels of the source. The presence of the CRSF has been long debated in X Persei. Its presence was first reported by Coburn et al. (2001) at $28.6_{-1.7}^{+1.5}$ keV, but was not confirmed later by the *BeppoSAX* and *INTEGRAL* observations. We report a strong evidence for the presence of the line at $38.6 \pm 4.4$ and $40.8 \pm 2.3$ keV, for the ‘High’ and ‘Int-2’ intensity levels, respectively. We however do not find a conclusive evidence for the presence of the line in the average spectrum. The detection of the CRSF at a higher centroid energy than in the *RXTE* observations might be related to the difference in intensity between the two by a factor of ~3. The centroid energy of the CRSF varies with intensity. A positive correlation with luminosity has been detected in several other low-luminosity sources like GX 304-1 and Her X-1 (Staubert et al. 2007; Yamamoto et al. 2011; Klochkov et al. 2012). The measured luminosity of X Persei being sub-critical, the source perfectly fits in this group. In the sub-critical accretion regime, the CRSF energy increases at higher intensities as the accretion mound is pushed more towards the surface of the neutron star with increasing ram pressure thereby sampling higher magnetic field (assuming a dipolar geometry for the magnetic field). The obtained result also points at another important aspect that the CRSF in X Persei is preferably detected at higher intensities. This was already hinted at Coburn et al. (2001) to explain why the CRSF feature was

not detected in the *BeppoSAX* observation. In Table 4, we list the 1–10 keV flux obtained from different observations of the source using different instruments. The results indicate that the CRSF is detected at higher intensities. In fact the *Suzaku* observation seems to have caught the source at the highest average intensity observed till now. The only other report is from the *XMM–Newton* observation of the source, which was reported to be at the same luminosity (La Palombara & Mereghetti 2007). However, the *XMM* band does not allow the detection of the CRSF.

The identification of the line centroid energy is one of the surest method to estimate the magnetic field strength of the emitting region in the neutron star. This is given by the ‘12-B-12’ rule providing an approximate relation between the observed CRSF energy and the magnetic field strength in the scattering region:

$$E_{\text{cyc}} = \frac{11.57 \text{ keV}}{1+z} \times B_{12} \quad (2)$$

where $B_{12}$ is the magnetic field in units of $10^{12}$ G and $z \sim 0.15$ is the gravitational redshift in the scattering region for standard neutron star parameters. This implies the magnetic field strength of the neutron star is $B = 3.4 \times 10^{12}$ G, assuming the scattering region lies close to the neutron star surface.

An intriguing aspect of the CRSF in X Persei is that the residuals after fitting the continuum model in the ‘Int-2’ level spectrum shows two dip-like structures, one at ~29 keV and the other at ~40 keV. This is an indication of the CRSF being non-Gaussian with a more complex shape. This aspect has been discussed before by Pottschmidt et al. (2005); Nakajima et al. (2010) and Mushtukov et al. (2015) for the accreting pulsar V 0332+53 where a similar effect has been observed. A complicated non-Gaussian CRSF shape has been long predicted by theory (Schönherr et al. 2007) but has not been confirmed convincingly from observational evidences, except for one source V0332+53. X Persei will only be the second source in this regard. This effect is also expected to be more prominent at lower luminosities as explained by several theories. Bhattacharya & Mukherjee (2011) predicted complicated CRSF shapes in the spectra of low-luminosity pulsars. This is due to the distortion of the dipolar magnetic field near the base of the accretion mound due to the effect of local instabilities. Mushtukov et al. (2015) also predicted a similar effect for sub-critical sources due to the variation of the doppler boost with changing luminosity as discussed before. The observed CRSF in the low-luminosity sub-critical source X Persei is consistent with these predictions. We encourage further deep observations of this source with sensitive instruments having high-energy resolution to probe this aspect deeper.

## 7 SUMMARY

We presented a detailed broad-band timing and spectral study of X Persei performed using a *Suzaku* observation. By testing different continuum models, we have obtained the representative broad-band X-ray spectrum of X Persei. The spectral fits indicate that BMC is a dominating factor for the Comptonization of the seed photons at the base of the accretion column; both indicated by the requirement of a high $\beta$ in the ‘COMPMAg’ model and a hard power-law tail-like feature with an exponential rollover at ~56 keV obtained with the ‘newhcut’ model. For the first time, we have identified different intensity levels of the source with distinct changes in the pulsation characteristics and the energy spectrum. All of these indicate a change in the accretion geometry of X Persei with varying intensity. We have also found evidence of a CRSF at ~40 keV at
higher intensities. This may be related to the fact that the CRSF is preferably detected at higher intensities, and may also indicate a correlation of the line centroid energy with intensity.

ACKNOWLEDGEMENTS

This work has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by the NASA Goddard Space Flight Center. CM acknowledges the hospitality from Nordita, KTH Royal Institute of Technology and Stockholm University for hosting her for a week, where most of the work for the paper was done and also acknowledges very fruitful discussions with Ruben Farinelli for help with the COMPMAG and COMPMAG2 models.

REFERENCES

Barlow R., 1989, Statistics. A Guide to the Use of Statistical Methods in the Physical Sciences. The Manchester Physics Series, Wiley, New York

Becker P. A., Wolff M. T., 2005, ApJ, 621, L45

Becker P. A., Wolff M. T., 2007, ApJ, 654, 435

Becker P. A. et al., 2012, A&A, 544, A123

Bhattacharya D., Mukherjee D., 2011, in Khare P., Ishwara-Chandra C. H., eds, ASP Conf. Ser. Vol. 3, Proc. of the 29th Meeting of the Astronomical Society of India. Astron. Soc. Pac., San Francisco, p. 25

Burnard D. J., Arons J., Klein R. I., 1991, ApJ, 367, 575

Chakrabarty D. et al., 1997, ApJ, 474, 414

Coburn W., 2001, PhD thesis, Univ. California

Coburn W., Heindl W. A., Gruber D. E., Rothschild R. E., Staubert R., Wilms J., Kreykenbohm I., 2001, ApJ, 552, 738

Delgado-Martí H., Levine A. M., Pfahl E., Rappaport S. A., 2001, ApJ, 546, 455

Di Salvo T., Burderi L., Robba N. R., Guainazzi M., 1998, ApJ, 509, 897

Doroshenko V., Santangelo A., Kreykenbohm I., Doroshenko R., 2012, A&A, 540, L1

Farinelli R. et al., 2012, MNRAS, 424, 2854

Farinelli R., Ferrigno C., Bozzo E., Becker P. A., 2016, A&A, 591, A29

Klochkov D. et al., 2008, A&A, 482, 907

Klochkov D. et al., 2012, A&A, 542, L28

La Palombara N., Mereghetti S., 2007, A&A, 474, 137

Lutovinov A., Tsygankov S., Chernyakova M., 2012, MNRAS, 423, 1978

Lyubimkov L. S., Rostopchin S. I., Roche P., Tarasov A. E., 1997, MNRAS, 286, 549

Makishima K., Mihara T., Nagase F., Tanaka Y., 1999, ApJ, 525, 978

Malacaria C., Klochkov D., Santangelo A., Staubert R., 2015, A&A, 581, A121

Mihara T., 1995, PhD thesis, Dept of Physics, Univ. Tokyo (M95)

Mitsuda K. et al., 2007, PASJ, 59, 1

Mushtukov A. A., Tsygankov S. S., Serber A. V., Suleimanov V. F., Poutanen J., 2015, MNRAS, 454, 2714

Nakajima M., Mihara T., Makishima K., 2010, ApJ, 710, 1755

Orlandini M., Frontera F., Masetti N., Sguera V., Sidoli L., 2012, ApJ, 748, 86

Postnov K. A., Gornostaev M. I., Klochkov D., Laplace E., Lukin V. V., Shakura N. I., 2015, MNRAS, 452, 1601

Pottschmidt K. et al., 2005, ApJ, 634, L97

Protassov R., van Dyk D. A., Connors A., Kashyap V. L., Siemiginowska A., 2002, ApJ, 571, 545

Schönherr G., Wilms J., Kretschmar P., Kreykenbohm I., Santangelo A., Rothschild R. E., Coburn W., Staubert R., 2007, A&A, 472, 353

Sguera V., Sidoli L., Bazzano A., Bassani L., Orlandini M., 2011, preprint (arXiv:1106.2067)

Shakura N., Postnov K., Kochetkova A., Hjalmarsdotter L., 2012, MNRAS, 420, 216

Staubert R., Shakura N. I., Postnov K., Wilms J., Rothschild R. E., Coburn W., Rodina L., Klochkov D., 2007, A&A, 465, L25

Tanaka Y., 1986, in Mihalas D., Winkler K.-H. A., eds, Lecture Notes in Physics Vol. 255, IAU Colloq. 89: Radiation Hydrodynamics in Stars and Compact Objects. Springer-Verlag, Berlin, p. 198

Telting J. H., Waters L. B. F. M., Roche P., Boogert A. C. A., Clark J. S., de Martino D., Persi P., 1998, MNRAS, 296, 785

Tsygankov S. S., Lutovinov A. A., Churazov E. M., Sunyaev R. A., 2007, Astron. Lett., 33, 368

White N. E., Mason K. O., Sanford P. W., 1977, Nature, 267, 229

White N. E., Swank J. H., Holt S. S., 1983, ApJ, 270, 711

Yamamoto T., Sugizaki M., Mihara T., Nakajima M., Yamaoka K., Matsuoka M., Morii M., Makishima K., 2011, PASJ, 63, S751

This paper has been typeset from a *TEX/LATEX* file prepared by the author.