Do massive neutron stars end as invisible dark energy objects?

Do massive neutron stars end as invisible dark energy objects?


Astronomical observations reveal a gap in the mass spectrum of relativistic objects: neither black holes nor neutron stars having masses in the range of 2 - 5 have ever been observed.
Based on the solution of the TOV equation modified to include a universal scalar field we argue that all moderate and massive neutron stars should end invisible dark energy objects (DEOs).

Triggered by the baryonic matter interaction, a phase transition from normal compressible nuclear matter into an incompressible quark-superfluid is shown to occur at roughly times the nuclear density. At the transition front, the scalar field is set to inject energy at the maximum possible rate via a non-local interaction potential This energy creates a global confining bag, inside which a sea of freely moving quarks is formed in line with the asymptotic freedom of quantum chromodynamics. The transition front, creeps from inside-to-outside to reach the surface of the object on the scale of Gyrs or even shorter, depending on its initial compactness. Having reached then the total injected dark energy via turns NSs into invisible DEOs.
While this may provide an explanation for the absence of stellar BHs with and NSs with , it also suggests that DEOs might have hidden connection to dark matter and dark energy in cosmology.


Keywords:  Relativity: general, black hole physics — neutron stars — superfluidity — QCD — dark energy — dark matter

1 Turbulent superfluidity in Neutron stars

The interiors of pulsars and NSs most likely are made of superfluids governed by triangular lattice of quantized vortices as prescribed by the Onsager-Feynman equation: here denote the velocity field, the vector of line-element, the reduced Planck constant and the mass of the superfluid particle pair, respectively.
Accordingly, the core of the Crab pulsar, should have approximately neutron and proton-vortices (Fig. 1). Let the evolution of the number density of vortex lines, , obey the following advection-diffusion equation:


where denote the transport velocity at the cylindrical radius and dissipative coefficient in the local frame of reference, respectively. When , then the radial component of in cylindrical coordinates reads: In the case of the Crab; this implies that approximately neutron vortices must be expulsed/annihilated each second, and therefore the object should switch off after up to yr, depending on the underlying mechanism of heat transport (see Baym, 1995; Link, 2012, and the references therein).

Figure 1: A magnetized neutron star with a superfluid core threaded by billions of vortex lines and magnetic flux tubes.

On the other hand, recent numerical calculations of superfluids reveal generation of large amplitude Kelvin waves that turn superfluids turbulent (see Baranghi, 2008; Baggaley & Laurie, 2014; Dix, 2014, and the references therein). It is therefore unlikely that trillions of Kilometer-long neutron and protons-vortices inside pulsars and NSs would behave differently. In this case, should be replaced by a mean turbulent velocity with being an upper limit3. As the number of vortex lines decreases with time due to emission of magnetic dipole radiation and therefore the separation between them increases non-linearly, it is reasonable to associate a time-dependent turbulent length scale which covers the two limiting cases: cm and This yields the geometrical mean Putting terms together and using to describe the effective turbulent viscosity, we obtain an upper limit for the global diffusion time scale: yr. Similarly, a comparable time scale for the Ohmic diffusion in this turbulent medium can be constructed as well. This is in line with observations, which reveal that most isolated luminous NSs known are younger than yr (see Espinoza, 2011, and the references therein). Assuming quantized vortices in NSs to obey a triangular lattice distribution, then the very central region would be the first to be evacuated from vortex lines and all other removable energies that do not contribute significantly to the pressure. Hence the radius of this region, would creep outwards with an average velocity: cm/s. The nuclear matter inside would be in the lowest possible energy state, which, as argued here, must be the incompressible quark-superfluid phase. Having reached then the NS turns invisible.
In analogy with normal massive luminous stars, massive and highly compact NSs appear to also switch-off earlier than their less massive counterparts (Hujeirat 2016). For alternative models explaining the above-mentioned mass gap see Belczynski (2012), Chapline (2014) and the references therein.

2 The onset of incompressibilitiy

Modeling the internal structure of cold NSs while constraining their masses and radii to observations, would require their central densities to inevitably be much higher than the nuclear density : a density regime in which all EOSs become rather uncertain and mostly acausal (see Hempel et al., 2011, and the references therein). This however can be viewed as a consequence of the considerable reduction of the compressibility of the nuclear matter at . To clarify this argument: Assume that the energy density and the pressure at have reached the critical state, at which the particle involved communicate with each other at the the maximum possible speed, e.g. the speed of light. This corresponds to the EOS: In this case, the the chemical potential equation reads:

Let the fast communicating particles occupy the finite central volume where is an arbitrary small radius. The particles involved practically form a fluid portion that cannot accept compression anymore, as otherwise the causality condition would be violated. The number density here would saturate around and yields a maximum local pressure With this and , the fluid portion inside is practically incompressible. On the other hand, the energy inside is uniform and the involved particles share the same energy, i.e. where But as then local pressure must vanish. This means that the validity of calculating the pressure from the chemical potential alone breaks down. As a consequence, using this formula in this regime would give rise to unrealistically high central energy densities and most likely would violate causality. Moreover, the regularity condition imposed on the pressure at r=0 enforces the supranuclear dense fluid inside to also be nearly incompressible. To explain this point: since the gradient of the pressure vanishes at the RHS of the TOV-equation (see Eq. 9) must vanish as well. This is feasible, if the enclosed mass becomes vanishingly small i.e. for On such small length scales and, in the absence of local or exotic feeding mechanisms, gravity alone cannot enforce to increase faster than as Therefore the spatial variation of inside remains limited, which means that and therefore the formation of the density plateau around becomes inevitable. Under these conditions, computing the local pressure from the chemical potential alone would yield an unrealistic The usual adopted strategy to escape this pressure-deficiency is to enforce an unfounded inward-increase of as resulting therefore in unreasonably large central densities.

3 The onset of quark-superfluidity

Another possible solution, which we propose here, runs as follows:

  • The nuclear matter at indeed reaches the compressibility limit and can be well-described by the stiffest EOS

  • A pure incompressible nuclear matter has a constant chemical potential and therefore the validity of computing the local pressure from the chemical potential alone breaks down. In such flows a non-local pressure for controlling the dynamics of the nuclear fluid is required.

  • The transition from compressible into pure-incompressible fluid phase might be provoked by the onset of a scalar field - matter interaction, which become active, once a critical density, is surpassed. The interaction potential, generates a non-local negative pressure which is capable of supporting the fluid-configuration against its own self-gravity.

  • The onset of interaction has a run-away character: injects dark energy, which in turn enforces the transition front to creep from inside-to-outside to abruptly terminate at the surface of the object.

Indeed, beyond , short-range repulsive interactions between particles mediated by the exchange of vector mesons most likely will dominate the dynamics of nuclear matter and would enhance the asymptotic convergence of the EOSs towards (see Haensel et al., 2007; Camenzind, 2007, and the references therein). The chemical potential here increases linearly with the number density of the baryonic matter This regime is classified here as H-State and depicted in red-color in Fig. (2).

Recalling that central densities, in NSs increase with their masses, but upper-bounded by to fit the observed mass function (see Lattimer, 2011, and the references therein), we conclude that the linear correlation must terminate at a certain critical density where attains a global maximum Baym & Chin (1976).

On the other hand, in an ever expanding universe, the eternal-state of matter should be the one at which the internal energy reaches a global minimum in spacetime (zero-temperature, zero-entropy and where Gibbs energy per baryon is lowest; henceforth the L-State). Taking into account that inside the object together with the a posteriori results (see Fig. 5), we conclude that and therefore the local pressure must vanish as well. In this case a non-local pressure must be generated in order to oppose self-collapse4of NSs into BHs with
If the transition layer between the H and L-states is of finite width in the space, then here may be positive, negative and/or discontinuous.
However, the case should be excluded, as it implies that the eternal state of matter would be more energetic than the H-State, which is a contradiction by constrcution. Similarly, the case is forbidden as it would violate energy conservation (; adding more particles yields a smaller pressure). Moreover, let us re-write the TOV equation in terms of :


Obviously, as a negative would destabilize the hydrostatic equilibrium, unless external sources are included, e.g. bag energy and/or external fields.
Therefore, although a first order phase transition may not be completely excluded, a crossover phase transition into an incompressible superfluid phase with would be more likely. Here, and on both sides of the transition front are equal and, with the help of an external field, both and across the front can be made even continuous (Fig. 2)).

In the present study, the simultaneous occurrence of the onset of baryonic matter interaction with the crossover phase transition is necessary in order to generate a non-local pressure with capable of opposing compression exerted by the surrounding curved spacetime. In the regime such a pressure may nicely resemble a non-local bag energy of quarks in the continuum.
In the presence of , the chemical potential per particle at would be upper-limited by the energy required for quark-deconfinement. In this case, the corresponding Gibbs function reads:


Based on our test calculations, an interaction potential obeying a power law distribution of the type: turns out to be optimal for maximizing the compactness of the compact object, i.e, where corresponds to the dynamical Schwarzschild radius (Fig. 5).

Figure 2: A schematic description of the chemical potential versus the number density at the centers of NSs. At a critical central density, the universal scalar field is set to provoke a crossover phase transition from compressible nuclear fluid into incompressible quark-superfluid. The transition front creeps from inside-to-outside to reach the surface of the object on the scale of Gyrs.

Subtituting and in Eq. (3) at , then reduces to:


The Gibbs function here may accept several minima at though doesn’t necessary vanish. However and should be excluded, as they are energetically unfavorable for smooth crossover phase transitions to occur.
On the other hand, by varying a set of true minima could be found. One way to constrain is to relate it to the canonical energy scale characterizing the effective coupling of quarks, i.e. (see Bethke, 2007, and the references therein). Indeed, as shown in Fig (3), attains a zero-minimum at for
The question to be addressed here is whether the above-mentioned localized analysis would apply for the whole object as well?
Indeed, the injected dark energy, via enforces the spacetime embedding the whole object to be increasingly curved, thereby maximizing the compression of the fluid in front of up to the critical limit and sets into an outward motion. The enclosed dark energy via grows with radius as i.e. faster than the growth of the baryonic mass, thereby enabling the object to reach a maximum compactness precisely at Note that the cases with and should be excluded. In the former case, the resulting objects must have collapsed into BHs with which have not been observed. The latter case is not supported by observation either as the surfaces of these massive NSs would continue to be dominated by a normal luminous matter.
Behind a sea of freely moving quarks is formed, though globally confined by the strongly curved spacetime surrounding the object, which acts as a global confining bag for the quarks. Note that, unlike the constant bag energy model of quarks, where the enclosed deconfinement energy scales linearly with the number of 3-quarks flavors , the injected dark energy in the present model scales as This extra-energy may be viewed as a mechanism for further enhancing the gluon like-field embedding the quark-continuum.

We may examine the conditions of coupling of particles in this pure quark-sea by setting and taking to be the number of quark flavors in the effective quark-gluon coupling constant:


Relating to Fermi momentum and use to infer the Fermi wave number we obtain

However, noting that the sea of quarks is incompressible in which communication between particles is mediated with the speed of light, we conclude that the value of should attain its true minimum, which is expected to be much smaller than Nevertheless, the present value of still ensures that quarks are in the safe energy regime, where they move almost freely in line with the asymptotic freedom of quantum chromodynamics -QCD (see Bethke, 2007, and the references therein).

Figure 3: The modified Gibbs function versus baryonic number density n (in units of ) is shown for various values of and Obviously, and appear to be the most appropriate parameters that are compatible with QCD. The value corresponds to the canonical energy scale characterizing the effective coupling of quarks inside individual hadrons. The Gibbs function here attains a zero-minimum at at which is set to provoke a phase transition into the INQSF state.

4 Governing equations and solution method

Our investigation here is based on numerical solving the TOV equation modified to include scalar fields The modified stress energy tensor reads:


The superscripts ”0” and ”” correspond to baryonic and scalar field tensors:


here is the 4-velocity, the subindices is a background metric of the form:


where are functions of the radius.
Assuming the configuration to be in hydrostatic equilibrium, then the GR field equations, reduce into the generalized TOV equations:


where is the total enclosed mass: and where
here denotes the interaction potential of the scalar field with the baryonic matter, i.e., the rate at which dark energy is injected into the system and is the time-derivative of

Figure 4: The radial distributions of the baryonic pressure () and negative pressure () inside an incompressible quark-superfluid core (left). The enclosed mass of the baryonic matter and the gradual mass-enhancement due to dark energy is shown for different values of (right).

Our reference object is a NS with with a radius where is the Schwarzschild radius. is assumed to be spatially and temporarily constant, whereas is set to obey the power-law distribution: and are constant parameters that are chosen so to fulfill the a posteriori requirement: for In most of the cases considered here, is set to be identical to the canonical energy scale at which mometum transfer between quarks saturates, i.e., GeV. The fluid in the post transition phase is governed by the EOS:
For a given central density, the solution procedure adopted here is based on integrating the equations for the pressure, enclosed mass and pseudo-gravitational potential from inside-to-outside, using either the first order Euler or fourth order Runge-Kutte integration methods.

Figure 5: In the top panel we show the radial distributions of the metric coefficients and inside a NS (; and ) and inside a DEO (; and ). Obviously, normal models of NSs have larger radii and considerably less compact than their DEO-counterparts, which can be inferred from the very limited spacial variations of and In the lower panel, the compactness of a typical DEO, expressed in terms of - is shown for different values of The object turns invisible if is calculated using and

Figure 6: The profiles of the total energy density the pressure induced by and the combined pressure versus radius are shown for different evolutionary epochs Inside : and whereas outside : and In each epoch, the object has an INQSF-core overlayed by a shell of normal compressible matter obeying a polytropic EOS. Obviously, the object appear to comfortably adjust itself to the mass-redistribution inside where matter is converted into INQSF.

Figure 7: Upper mass limit of DEOs versus critical density (in units of ) is shown. The baryon interaction is set to occur at which in turn provokes the phase transition into the INQSF state. The most probable mass-regime of DEOs is marked here as a blue region. Accordingly, the progenitor of a DEO with should be a NS of provided it has an initial compactness and Similarly, a Hulse-Taylor type pulsar would end as a DEO of if its initial compactness is and if On the other hand, moderate and massive NSs with initial compactness i.e., need less dark energy to become invisible DEOs, but require unreasonably high for the onset of matter interaction. NSs falling in this category are to be compared with the colored small cycles and triangles, which show the approximate locations of various NS-models as depicted in Fig. (4) of Lattimer & Prakash (2011).

Figure 8: A schematic description of a DEO, inside which spacetime is fairly flat, but becomes extra-ordinary curved across their surfaces. As the binding energy inside DEOs vanishes, they are astoundingly similar to ultra-giant hadrons trapped inside a strongly curved spacetime, which render them invisible.

5 Results & discussions

The here-presented model of DEOs is motivated by the following three unresolved theoretical and observational problems in the astrophysics of NSs:

  • Why neither NSs nor BHs have ever been observed in the mass-range 2 - 5

  • Most sophisticated EOS used to model the internal structure of NSs are based on central densities that are far beyond the nuclear density: a density regime of great uncertainty.

  • How NSs end their life in an ever expanding universe and whether there is a hidden connection between the missing massive NSs and dark matter on the one hand and with dark energy in the universe on the other hand.

In this paper we argue that the formation of DEOs may provide answers to these unresolved problems. This scenario could be summarized as follows:

  1. The very central regions of NSs are made of superfluid nuclear matter and that these would be the first to be evacuated from vortex lines and all other removable energies that do not contribute significantly to the pressure. The nuclear fluid here is governed by the stiff EOS:

  2. In order to escape collapse into a BH with the chemical potential in the very central regions cannot grow indefinitely, and it must terminate at a certain critical value, where the fluid is set to undergo a phase transition.
    Based on minimum energy consideration, a crossover phase transition into an incompressible quark-superfluid has been shown to be energetically a favorable transition.

  3. We have shown that in the presence of a universal scalar field the injected dark energy is capable of provoking a phase transition into INQSF that roughly occurs at The action of the injected energy is equivalent to generating a gluon-like field, or enhance the available gluon-field through forming a global energy bag in the continuum, inside which quarks move almost free in line with the asymptotic freedom of quantum chromodynamics.

  4. We have shown that the transition front creeps from inside-to-outside on the scale of Gyrs, forming a sea of quarks behind the front. Indeed, the very slow outwards propagation of grants the NS ample of time to stably react to all possible conditions associated with the phase transition, including a global re-distribution of mass inside (Fig. 6).

  5. We have shown that an interaction potential of the type is capable of maximizing the compactness of the object (Fig. 5).

  6. Having reached the surface of the NSs, these object become DEOs. Their interiors are made solely of INQSFs with constant chemical potential. The spacetime inside DEOs has been identified to be fairly flat, whereas it promptly becomes extra-ordinary curved across their surfaces (Fig. 5). Inside DEOs, the nuclear fluid has a vanishing binding energy and therefore mimicking the configuration of an ultra-giant hadron trapped in a strongly curved spacetime.

  7. According to the here-presented scenario, all visible pulsars and NSs must contain incompressible quark-superfluid cores supported and confined by a dark energy component which is induced by a scalar field of universal origin. The gravitational significance of the injected dark energy in these cores depends strongly on their evolutionary phase and in particular on their ages and initial compactness. Accordingly, young NSs should be less massive than old ones, and the very old NSs should turn invisible by now.
    To quantify the mass-enhancement by let be the mass of the NS at its birth and being the mass enhancement due to . Requiring then the following inequality holds:


    or equivalently,


    where denote the total energy, the density in units of g/cc and the baryoinc mass of the NS in units of respectively.
    Thus, NSs are born with and by interacting with they become more massive and more compact to finally reach at the end of their luminous phase, which would last for approximately yr or less, depending on their initial compactness. Thus, a NS with initial compactness will have to double its mass to become a DEO (Fig. 4 and Fig. 7).
    According to the present scenario, the Hulse-Taylor pulsar should have an INQSF core, though the dark energy component is gravitationally insignificant due to its young age, and therefore the size of its INQSF-core must be still small. Assuming the baryon mass of the pulsar to remain constant as it evolve on the cosmological time scale, then the pulsar will turn into invisible-DEO in roughly one Gyr. This would imply that the onset of baryon interaction should occur at roughly four times the nuclear density, which is in the range of the here-predicated critical density (Fig. 3). On the other hand, the extra-mass resembles the lower energy limit required for deconfining the sea of quarks, i.e., the energy needed for generating a see of quark anti-quark pairs. Similar to quarks in hadrons, the sea of quarks inside DEOs can never be observed as free objects in the sky.

Recalling that the effective potential of the gluon-field inside individual hadrons is on the average predicted to increases with radius as and that the spatial variation of the coefficient of the Schwarzschild metric on comparable length scales is negligibly small (), we conclude that gluon-fields do not accept stratification by gravitational fields.
Therefore as in the present DEO-models is dominant and increases with radius, the sea of quarks inside DEOs is in a purely incompressible state and cannot accept stratification (see in Fig. 5). In such gravitationally bounded incompressible fluid-configurations, not only that but the classical repulsive pressure must vanish also and should be replaced by a non-local pressure, in order to avoid the formation of BHs with

Unlike EOSs in compressible normal plasmas, classical EOSs in incompressible superfluids are non-local. In the latter case, constructing a communicator that merely depends on local exchange of information generally would not be sufficient for efficiently coupling different/remote parts of the fluid in a physically consistent manner. A relevant example is the solution of the TOV-equation for classical incompressible fluids . In this case, the pressure depends, not only on the global compactness of the object, but it becomes even acausal whenever the global compactness is enhanced.
This is similar to the case when solving the incompressible Navier-Stokes equations, where an additional Laplacian operator for describing the spatial variation of a non-local scalar field is constructed to generate a pseudo-pressure (; actually a Lagrangian multiplier), which, again, does not respect causality Hujeirat & Thielemann (2009).

Indeed, DEOs made of incompressible quark-superfluids would be stable also against mass-enhancement from outside. Let a certain amount of baryonic matter, be added to the object from outside. Then the relative increase of compared to scales as: where is the average density of the newly settled matter. Unless which is forbidden under normal astrophysical conditions, the star would react stably. However, in the case of super-Eddington accretion or merger, the newly settled matter must first decelerate, compressed and subsequently becomes virially hot, giving rise therefore to On the other hand, such events would lower the confinement stress at the surface and would turn the quantum jump of the energy density at which falls abruptly from approximately erg/cc at down to zero outside it, into an extra-ordinary steep pressure gradient in the continuum. While such actions would smooth the strong curvature of spacetime across they would enable DEOs to eject quark matter into space with ultra-relativistic speeds, which is forbidden. Nonetheless, even if this would occur instantly, then the corresponding time scale would be of order where is the jump width in centimeters and c is the speed of light. Relating to the average spacing between two arbitrary particles this yields s, which is many orders of magnitude shorter than any known thermal relaxation time scale between arbitrary luminous particles.

Although electromagnetic activities and jets have not been observed in dark matter halos, they are typical events for systems containing black holes. Recalling that supermasive GBECs are dynamically unstable Hujeirat (2012), our results here address the following two possibilities:

  • If the onset of -baryon interaction indeed occurs at then the majority of the first generation of stars and the massive stars formed in the subsequent early epochs must have ended as pulsars and NSs, rather than collapsing into stellar BHs with . In this case, dark matter halos most likely should be DEO-rich clusters. These clusters must have been extraordinary luminous in the early universe, but became inactive and dark after the nuclear matter in the interiors of NSs converted into the INQSF-phase, subsequently sweeping away all sorts of luminous matter in their surroundings due to their inability to accrete normal matter. The enormous surface stress confining the sea of quarks in the interiors of DEOs render their surfaces impenetrable for normal matter, hence these objects behave as non-interacting objects.

  • The average repulsive forces governing clusters of DEOs most likely would enforce approaching luminous matter to deviate from face-to-face collisions and therefore stay inactive, though n-body and SPH-numerical calculations are needed here to verify this argument.

Finally we note that, similar to the gluon field confining and governing the dynamics of almost massless quarks in hadrons, the induced energy enhancement of the gluon-like field in DEOs cannot surpass the limit, beyond which they collapse to form BHs with Moreover, the enclosed dark energy injected via scales as : this outlines an upper limit for the increase of confining energy with radius in DEOs, beyond which they undergo a self-collapse. However, whether this limit applies for the potential of the gluon field inside hadrons is not clear at the moment and demands further investigations.

In a subsequent article, we discuss the compatibility and physically consistency of the here-presented internal structures of DEOs with the bi-metric formulation of spacetime in general relativity proposed by Rosen (1977).

Acknowledgment The author thanks Johanna Stachel, Friedel Thielemann, James Lattimer, George Chapline, Tsvi Piran, Juergen Berges, Jan Martin Pawlowski, Max Camenzind, Ravi Samtaney and Matthias Hempel for the very helpful comments and useful discussions on various aspects of this article.


  1. pagerange: Do massive neutron stars end as invisible dark energy objects?LABEL:lastpage
  2. pubyear: 2002
  3. The rotational energy associated with the outward-transported vortex lines from the central regions are turbulently re-distributed in the outer shells and should not necessary suffer a complete annihilation.
  4. An incompressible fluid with has a negative local pressure. Therefore an acausal non-local pressure is necessary for stabilizing the configuration.


  1. Alpar, M.A., Anderson, P.W., Pines, D., Shaham, J., ApJ, 278, 791, 1984
  2. Baggaley, A.W., Laurie, J., Phys. Rev. B., 89, 014504, 2014
  3. Baym, G., Nuclear Physics A, 233, 1995
  4. Baym, G., Chin, S.A., Phys. Lett. 62B, 241, 1976
  5. Baranghi, C., Physica D, 237, 2195, 2008
  6. Belczynski, K., Wiktorowicz, G., Fryer, C., et al., ApJ, 757, 91, 2012
  7. Bethke, S., Progress in Particle and Nuclear Physics, 351, 58, 2007 Belczynski, S., Progress in Particle and Nuclear Physics, 351, 58, 2007
  8. Camenzind, M., ”Compact Objects in Astrophysics”, Springer, 2007
  9. Chapline, G., Barbieri, J., International Journal of Modern Physics D, 23, No. 3, 1450025, 2014
  10. Dix, O.M., Zieve, R.J., Physical Review B, 144511, 90, 2014
  11. Espinoza, C.M., Lyne, A.G., Stappers, B.W., Kramer, C., MNRAS, 414, 1679, 2011
  12. Hampel, M., Fischer, T., et al., ApJ, 748, 70, 2012
  13. Haensel, P., Potekhin, A.Y. & Yakovlev, D.G., ”Neutron stars 1”, Springer, 2007
  14. Hujeirat, A.A., Thielemann, F-K., MNRAS, 400, 903, 2009
  15. Hujeirat, A.A., MNRAS, 423.2893, 2012
  16. Hujeirat, A.A., in preparation, 2016
  17. Kalogera, V., Baym, G., APJ, 470, L61, 1996
  18. Lattimer, J.M., Prakash, M., in ”From Nuclei To Stars”, Ed. S. Lee, World Scientific Publishing, Singapur, 2011
  19. Link, B., MNRAS, 422, 1640, 2012
  20. Rosen, N., ApJ, 211, 357, 1977
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description