The orientation and evolution based on unified scheme for jetted extragalactic radio sources posi... more The orientation and evolution based on unified scheme for jetted extragalactic radio sources posits that BL Lacertae objects (BLs), flat-spectrum radio quasars (FSRQs) and normal radio galaxies (RGs) represent increasingly misaligned populations of active galactic nuclei (AGNs). Using compiled radio, X-ray and γ-ray data of 397 blazars and 110 RGs from the Fermi Large Area Telescope (Fermi-LAT) catalogue, we computed the viewing angles, γ-ray core-dominance parameter and γ-ray emission components in order to study the consequences of orientation and relativistic beaming effects on γ-ray properties of RGs, BLs and FSRQs. Our results show continuous distributions of core-dominance parameters (X-ray, RX and γ-ray, Rγ) from RGs at low values, largest viewing angles to FSRQs at high values and BLs subsets with the least values. The difference on the plane is significantly larger for FSRQs and BLs than for RGs, indicating an evolutionary link between them. A two-sample Wilcoxon rank-sum and Kolmogorov-Smirnov tests carried out on our data suggest that the probabilities of the distribution of RX and Rγ of RGs and blazar types to come from the same parent distribution are pWRS ∼ 0 and pK−S < 10-5, suggestive of stronger beaming effects in blazars than in RGs. There is a significant correlation (r > 0.60) between log Rr - log RX for the combined sample types. Furthermore, a significant anti-correlation (r ∼ -0.80) exists in the log Rγ - log Lγ,un plot which is indicative of evolutionary sequence via relativistic beaming model. These results imply that the evolutionary track of jetted AGNs is RGs - BLs FSRQs
The unified scheme of Seyfert galaxies hypothesizes that the observed differences between the two... more The unified scheme of Seyfert galaxies hypothesizes that the observed differences between the two categories of Seyfert galaxies, type 1 (Sy1) and type 2 (Sy2) are merely due to the difference in the orientation of the toroidal shape of the obscuring material in the active galactic nuclei. We used in this paper, a sample consisting of 120 Seyfert galaxies at 1.40 × 109 Hz in radio, 2.52 × 1017 Hz in X-ray and 2.52 × 1023 Hz in γ-ray luminosities observed by the Fermi Large Area Telescope (Fermi- LAT) in order to test the unified scheme of radio-quiet Seyfert galaxies. Our main results are as follows: (i) We found that the distributions of multiwave luminosities (Lradio, LX-ray, and Lγ-ray) of Sy1 and Sy2 are completely overlapped with up to a factor of 4. The principal component analysis result reveals that Sy1 and Sy2 also occupy the same parameter spaces, which agrees with the notion that Sy1 and Sy2 are the same class objects. A Kolmogorov-Smirnov test performed on the sub-sample...
The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the ye... more The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the years. Though a consensus has not been reached with regards to the actual cause of the phenomenon, the electromagnetic braking torque on the crust quantified via the magnitude of pulsar spin frequency first derivative,ν is a key factor in mechanisms put across toward the understanding of the underlying principles involved. The glitch size has been used to establish a quantity used to constrain the mean possible change in pulsar spin frequency (ν) per year due to a glitch known as the 'glitch activity'. Traditionally, the glitch activity parameter A g is calculated from the cumulative glitch sizes in a pulsar at a certain observational time span. In this analysis, we test the possibility of quantifying the A g with the pulsars main spin frequency derivatives (i.e.ν andν). In this approach, the ratio of the frequency derivatives, i.e. |ν|/ν 2 is seen to constrains the glitch activity in radio pulsars. The glitch size is found to be independent of the magnitude of the ratio, however, based on the recorded glitch events, the lower end of the |ν|/ν 2 distribution appears to have more glitches. The minimum inter-glitch time interval in the ensemble of pulsars scale with the ratio as t g ∼ 3.35(|ν|/ν 2) 0.23. The A g quantified in this analysis supports the idea of neutron star inner-crust superfluid being the reservoir of momentum transferred during glitches. It suggests that the moment of inertia of the inner crust to be at most 10% of the entire neutron star moment of inertia.
The Star Formation Rate (SFR) of M83 galaxy was investigated. The first hand photometry data usin... more The Star Formation Rate (SFR) of M83 galaxy was investigated. The first hand photometry data using R, B, V and Hα filters was collected using 1.0m telescope for two nights. IRAF, Python and Sextractor software were used during data reduction and analysis. A scaling factor for R-band to Hα band counts was derived to be 0.043 while count/sec was found to be 2.98 x 10-20ergs-1 cm-2 −1 A . The Sextractor was used to identify the HII regions at the South-West (S-W) portion of the galaxy with a total of 1198.57 counts. This yielded a total of 1 2 1 6.44 10− − − × ergcm A Hα-flux per year. The derived total Hα luminosity for the same portion (S-W) is 4 1 1.21 10 − × ergs , which gave SFR of 0.95M⊙yr-1 and Dust Mass (DM) of (1.21 ± 0.02) x 107 Mo. The complete galaxy images observed with R-, V- and B- band filters were used for image reconstruction. The Hα luminosity, Hα SFR and DM presented here is suggested to be lower limits since they were not corrected for air mass and dust extinction.
The angular momentum transfer mechanism of pulsar glitches for over four decades now stands as st... more The angular momentum transfer mechanism of pulsar glitches for over four decades now stands as standalone theory with regards to glitch sizes and inter-glitch time intervals. However, recent analyses both analytic and statistical are on the verge of suppressing the theory. In this paper, we overviewed the superfluid theory to highlight the efficacy of the angular momentum process and highlighted the theoretical and observational evidences that could not be explained by processes involving transfer of angular momentum.
The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the ye... more The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the years. Though a consensus has not been reached with regards to the actual cause of the phenomenon, the electromagnetic braking torque on the crust quantified via the magnitude of pulsar spin frequency first derivative,ν is a key factor in mechanisms put across toward the understanding of the underlying principles involved. The glitch size has been used to establish a quantity used to constrain the mean possible change in pulsar spin frequency (ν) per year due to a glitch known as the 'glitch activity'. Traditionally, the glitch activity parameter A g is calculated from the cumulative glitch sizes in a pulsar at a certain observational time span. In this analysis, we test the possibility of quantifying the A g with the pulsars main spin frequency derivatives (i.e.ν andν). In this approach, the ratio of the frequency derivatives, i.e. |ν|/ν 2 is seen to constrains the glitch activity in radio pulsars. The glitch size is found to be independent of the magnitude of the ratio, however, based on the recorded glitch events, the lower end of |ν|/ν 2 distribution appear to have more glitches. The minimum inter-glitch time interval in the ensemble of pulsars scale with the ratio as t g ∼ 3.35(|ν|/ν 2) 0.23. The A g quantified in this analysis supports the idea of neutron star inner-crust superfluid being the reservoir of momentum transferred during glitches. It suggests that the moment of inertia of the inner-crust to be at most 10% of the entire neutron star moment of inertia.
The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the ye... more The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the years. Though a consensus has not been reached with regards to the actual cause of the phenomenon, the electromagnetic braking torque on the crust quantified via the magnitude of pulsar spin frequency first derivative,ν is a key factor in mechanisms put across toward the understanding of the underlying principles involved. The glitch size has been used to establish a quantity used to constrain the mean possible change in pulsar spin frequency (ν) per year due to a glitch known as the 'glitch activity'. Traditionally, the glitch activity parameter A g is calculated from the cumulative glitch sizes in a pulsar at a certain observational time span. In this analysis, we test the possibility of quantifying the A g with the pulsars main spin frequency derivatives (i.e.ν andν). In this approach, the ratio of the frequency derivatives, i.e. |ν|/ν 2 is seen to constrains the glitch activity in radio pulsars. The glitch size is found to be independent of the magnitude of the ratio, however, based on the recorded glitch events, the lower end of the |ν|/ν 2 distribution appears to have more glitches. The minimum inter-glitch time interval in the ensemble of pulsars scale with the ratio as t g ∼ 3.35(|ν|/ν 2) 0.23. The A g quantified in this analysis supports the idea of neutron star inner-crust superfluid being the reservoir of momentum transferred during glitches. It suggests that the moment of inertia of the inner crust to be at most 10% of the entire neutron star moment of inertia.
Strange Nuggets are believed to be among the relics of the early universe. They appear as dark ma... more Strange Nuggets are believed to be among the relics of the early universe. They appear as dark matter due to their low charge-to-mass ratio. Their distribution is believed to be the same as that of dark matter. As such, they could be accreted by high magnetic field objects and their collisions with pulsars are inevitable. Pulsar glitches are commonly seen as sudden spin-ups in pulsar frequency. It is still an open debate with regard to mechanisms giving rise to such a phenomenon. However, there is a class of sudden changes in pulsar spin frequency known as microglitches. These event are characterized by sudden small change in pulsar spin frequency ( δ ν / ν ≈ ± 10 − 9 $\delta \nu/\nu \approx \pm 10^{-9}$ ). Clearly, the negative signature seen in some of the events is inconsistent with the known glitch mechanisms. In this analysis, we suggest that accretion of strange nuggets with pulsars could readily give rise to microglitch events. The signature of the events depends on the energ...
Pulsar glitches are sudden spin-ups in pulsar spin frequency ($\nu$). The glitch size, $\Delta\nu... more Pulsar glitches are sudden spin-ups in pulsar spin frequency ($\nu$). The glitch size, $\Delta\nu/\nu$, is a key parameter in any mechanism puts across towards the understanding of the events.However, the distribution of the glitch sizes has persistently been bimodal.This bimodal nature could be intrinsic or otherwise. In this paper, the glitch size distribution is bisected at $\Delta\nu/\nu = 10^{-7}$ with $\Delta\nu/\nu 10^{-7}$ are taken as large size glitches (LSG).The magnitude of SSGis scaled to that of LSG and tested for this http URL pulsars with mixture of glitch sizes, Lilliefore test is used to identify the distribution pattern of SSGs and LSGs in such pulsars. The result indicates that each half of the size distribution is fundamentally different from one another. LSGs are seen to be normally distributed, while the SSGs are lognormal.
The orientation and evolution based on unified scheme for jetted extragalactic radio sources posi... more The orientation and evolution based on unified scheme for jetted extragalactic radio sources posits that BL Lacertae objects (BLs), flat-spectrum radio quasars (FSRQs) and normal radio galaxies (RGs) represent increasingly misaligned populations of active galactic nuclei (AGNs). Using compiled radio, X-ray and γ-ray data of 397 blazars and 110 RGs from the Fermi Large Area Telescope (Fermi-LAT) catalogue, we computed the viewing angles, γ-ray core-dominance parameter and γ-ray emission components in order to study the consequences of orientation and relativistic beaming effects on γ-ray properties of RGs, BLs and FSRQs. Our results show continuous distributions of core-dominance parameters (X-ray, RX and γ-ray, Rγ) from RGs at low values, largest viewing angles to FSRQs at high values and BLs subsets with the least values. The difference on the plane is significantly larger for FSRQs and BLs than for RGs, indicating an evolutionary link between them. A two-sample Wilcoxon rank-sum and Kolmogorov-Smirnov tests carried out on our data suggest that the probabilities of the distribution of RX and Rγ of RGs and blazar types to come from the same parent distribution are pWRS ∼ 0 and pK−S < 10-5, suggestive of stronger beaming effects in blazars than in RGs. There is a significant correlation (r > 0.60) between log Rr - log RX for the combined sample types. Furthermore, a significant anti-correlation (r ∼ -0.80) exists in the log Rγ - log Lγ,un plot which is indicative of evolutionary sequence via relativistic beaming model. These results imply that the evolutionary track of jetted AGNs is RGs - BLs FSRQs
The unified scheme of Seyfert galaxies hypothesizes that the observed differences between the two... more The unified scheme of Seyfert galaxies hypothesizes that the observed differences between the two categories of Seyfert galaxies, type 1 (Sy1) and type 2 (Sy2) are merely due to the difference in the orientation of the toroidal shape of the obscuring material in the active galactic nuclei. We used in this paper, a sample consisting of 120 Seyfert galaxies at 1.40 × 109 Hz in radio, 2.52 × 1017 Hz in X-ray and 2.52 × 1023 Hz in γ-ray luminosities observed by the Fermi Large Area Telescope (Fermi- LAT) in order to test the unified scheme of radio-quiet Seyfert galaxies. Our main results are as follows: (i) We found that the distributions of multiwave luminosities (Lradio, LX-ray, and Lγ-ray) of Sy1 and Sy2 are completely overlapped with up to a factor of 4. The principal component analysis result reveals that Sy1 and Sy2 also occupy the same parameter spaces, which agrees with the notion that Sy1 and Sy2 are the same class objects. A Kolmogorov-Smirnov test performed on the sub-sample...
The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the ye... more The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the years. Though a consensus has not been reached with regards to the actual cause of the phenomenon, the electromagnetic braking torque on the crust quantified via the magnitude of pulsar spin frequency first derivative,ν is a key factor in mechanisms put across toward the understanding of the underlying principles involved. The glitch size has been used to establish a quantity used to constrain the mean possible change in pulsar spin frequency (ν) per year due to a glitch known as the 'glitch activity'. Traditionally, the glitch activity parameter A g is calculated from the cumulative glitch sizes in a pulsar at a certain observational time span. In this analysis, we test the possibility of quantifying the A g with the pulsars main spin frequency derivatives (i.e.ν andν). In this approach, the ratio of the frequency derivatives, i.e. |ν|/ν 2 is seen to constrains the glitch activity in radio pulsars. The glitch size is found to be independent of the magnitude of the ratio, however, based on the recorded glitch events, the lower end of the |ν|/ν 2 distribution appears to have more glitches. The minimum inter-glitch time interval in the ensemble of pulsars scale with the ratio as t g ∼ 3.35(|ν|/ν 2) 0.23. The A g quantified in this analysis supports the idea of neutron star inner-crust superfluid being the reservoir of momentum transferred during glitches. It suggests that the moment of inertia of the inner crust to be at most 10% of the entire neutron star moment of inertia.
The Star Formation Rate (SFR) of M83 galaxy was investigated. The first hand photometry data usin... more The Star Formation Rate (SFR) of M83 galaxy was investigated. The first hand photometry data using R, B, V and Hα filters was collected using 1.0m telescope for two nights. IRAF, Python and Sextractor software were used during data reduction and analysis. A scaling factor for R-band to Hα band counts was derived to be 0.043 while count/sec was found to be 2.98 x 10-20ergs-1 cm-2 −1 A . The Sextractor was used to identify the HII regions at the South-West (S-W) portion of the galaxy with a total of 1198.57 counts. This yielded a total of 1 2 1 6.44 10− − − × ergcm A Hα-flux per year. The derived total Hα luminosity for the same portion (S-W) is 4 1 1.21 10 − × ergs , which gave SFR of 0.95M⊙yr-1 and Dust Mass (DM) of (1.21 ± 0.02) x 107 Mo. The complete galaxy images observed with R-, V- and B- band filters were used for image reconstruction. The Hα luminosity, Hα SFR and DM presented here is suggested to be lower limits since they were not corrected for air mass and dust extinction.
The angular momentum transfer mechanism of pulsar glitches for over four decades now stands as st... more The angular momentum transfer mechanism of pulsar glitches for over four decades now stands as standalone theory with regards to glitch sizes and inter-glitch time intervals. However, recent analyses both analytic and statistical are on the verge of suppressing the theory. In this paper, we overviewed the superfluid theory to highlight the efficacy of the angular momentum process and highlighted the theoretical and observational evidences that could not be explained by processes involving transfer of angular momentum.
The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the ye... more The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the years. Though a consensus has not been reached with regards to the actual cause of the phenomenon, the electromagnetic braking torque on the crust quantified via the magnitude of pulsar spin frequency first derivative,ν is a key factor in mechanisms put across toward the understanding of the underlying principles involved. The glitch size has been used to establish a quantity used to constrain the mean possible change in pulsar spin frequency (ν) per year due to a glitch known as the 'glitch activity'. Traditionally, the glitch activity parameter A g is calculated from the cumulative glitch sizes in a pulsar at a certain observational time span. In this analysis, we test the possibility of quantifying the A g with the pulsars main spin frequency derivatives (i.e.ν andν). In this approach, the ratio of the frequency derivatives, i.e. |ν|/ν 2 is seen to constrains the glitch activity in radio pulsars. The glitch size is found to be independent of the magnitude of the ratio, however, based on the recorded glitch events, the lower end of |ν|/ν 2 distribution appear to have more glitches. The minimum inter-glitch time interval in the ensemble of pulsars scale with the ratio as t g ∼ 3.35(|ν|/ν 2) 0.23. The A g quantified in this analysis supports the idea of neutron star inner-crust superfluid being the reservoir of momentum transferred during glitches. It suggests that the moment of inertia of the inner-crust to be at most 10% of the entire neutron star moment of inertia.
The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the ye... more The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the years. Though a consensus has not been reached with regards to the actual cause of the phenomenon, the electromagnetic braking torque on the crust quantified via the magnitude of pulsar spin frequency first derivative,ν is a key factor in mechanisms put across toward the understanding of the underlying principles involved. The glitch size has been used to establish a quantity used to constrain the mean possible change in pulsar spin frequency (ν) per year due to a glitch known as the 'glitch activity'. Traditionally, the glitch activity parameter A g is calculated from the cumulative glitch sizes in a pulsar at a certain observational time span. In this analysis, we test the possibility of quantifying the A g with the pulsars main spin frequency derivatives (i.e.ν andν). In this approach, the ratio of the frequency derivatives, i.e. |ν|/ν 2 is seen to constrains the glitch activity in radio pulsars. The glitch size is found to be independent of the magnitude of the ratio, however, based on the recorded glitch events, the lower end of the |ν|/ν 2 distribution appears to have more glitches. The minimum inter-glitch time interval in the ensemble of pulsars scale with the ratio as t g ∼ 3.35(|ν|/ν 2) 0.23. The A g quantified in this analysis supports the idea of neutron star inner-crust superfluid being the reservoir of momentum transferred during glitches. It suggests that the moment of inertia of the inner crust to be at most 10% of the entire neutron star moment of inertia.
Strange Nuggets are believed to be among the relics of the early universe. They appear as dark ma... more Strange Nuggets are believed to be among the relics of the early universe. They appear as dark matter due to their low charge-to-mass ratio. Their distribution is believed to be the same as that of dark matter. As such, they could be accreted by high magnetic field objects and their collisions with pulsars are inevitable. Pulsar glitches are commonly seen as sudden spin-ups in pulsar frequency. It is still an open debate with regard to mechanisms giving rise to such a phenomenon. However, there is a class of sudden changes in pulsar spin frequency known as microglitches. These event are characterized by sudden small change in pulsar spin frequency ( δ ν / ν ≈ ± 10 − 9 $\delta \nu/\nu \approx \pm 10^{-9}$ ). Clearly, the negative signature seen in some of the events is inconsistent with the known glitch mechanisms. In this analysis, we suggest that accretion of strange nuggets with pulsars could readily give rise to microglitch events. The signature of the events depends on the energ...
Pulsar glitches are sudden spin-ups in pulsar spin frequency ($\nu$). The glitch size, $\Delta\nu... more Pulsar glitches are sudden spin-ups in pulsar spin frequency ($\nu$). The glitch size, $\Delta\nu/\nu$, is a key parameter in any mechanism puts across towards the understanding of the events.However, the distribution of the glitch sizes has persistently been bimodal.This bimodal nature could be intrinsic or otherwise. In this paper, the glitch size distribution is bisected at $\Delta\nu/\nu = 10^{-7}$ with $\Delta\nu/\nu 10^{-7}$ are taken as large size glitches (LSG).The magnitude of SSGis scaled to that of LSG and tested for this http URL pulsars with mixture of glitch sizes, Lilliefore test is used to identify the distribution pattern of SSGs and LSGs in such pulsars. The result indicates that each half of the size distribution is fundamentally different from one another. LSGs are seen to be normally distributed, while the SSGs are lognormal.
Uploads
Papers by Innocent Eya