From <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mi>U</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo stretchy="false">)</mml:mo> <mml:mo>×</mml:mo> <mml:mi>U</mml:mi> <mml:mo stretchy="fals

We study the cosmology of a modified Majoron model motivated by the need to protect a global <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"> <a:mi>U</a:mi> <a:mo stretchy="false">(</a:mo> <a:mn>1</a:mn> <a:mo stretchy="false">)</a:mo> </a:math> symmetry from gravity-induced hard explicit breaking (by <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"> <e:mi>d</e:mi> <e:mo>≤</e:mo> <e:mn>4</e:mn> </e:math> operators) at the Planck scale. The model extends the standard model by introducing a gauged <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"> <g:mi>U</g:mi> <g:mo stretchy="false">(</g:mo> <g:mn>1</g:mn> <g:msub> <g:mo stretchy="false">)</g:mo> <g:mrow> <g:mi>B</g:mi> <g:mo>−</g:mo> <g:mi>L</g:mi> </g:mrow> </g:msub> </g:math> and an approximate global <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"> <k:mi>U</k:mi> <k:mo stretchy="false">(</k:mo> <k:mn>1</k:mn> <k:mo stretchy="false">)</k:mo> </k:math> symmetry, each spontaneously broken by a corresponding complex scalar singlet. This setup gives rise to a network of effectively global and local cosmic strings, whose stochastic gravitational wave signals can jointly account for the spectrum observed by NANOGrav collaboration, particularly for Majoron masses <o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"> <o:msub> <o:mi>m</o:mi> <o:mi>χ</o:mi> </o:msub> <o:mo>&lt;</o:mo> <o:msup> <o:mn>10</o:mn> <o:mrow> <o:mo>−</o:mo> <o:mn>23</o:mn> </o:mrow> </o:msup> <o:mtext> </o:mtext> <o:mtext> </o:mtext> <o:mi>eV</o:mi> </o:math> . Although the fit is not as strong as that from supermassive black hole mergers, the model still provides an alternative explanation rooted in high-energy physics. The Majoron mass induces an infrared cutoff in the gravitational wave spectrum, and we examine how this effect shapes the fit to the NANOGrav data. The model also generates light neutrino masses via the seesaw mechanism and avoids cosmological constraints from <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"> <q:mi mathvariant="normal">Δ</q:mi> <q:msub> <q:mi>N</q:mi> <q:mi>eff</q:mi> </q:msub> </q:math> , cosmic microwave background (CMB) anisotropies, and isocurvature fluctuations. Although the Majoron can contribute to dark matter through thermal, coherent oscillation, and string-induced production mechanisms, its relic abundance remains subdominant in the NANOGrav-compatible region. In contrast, the measured dark matter relic density is achievable at higher <t:math xmlns:t="http://www.w3.org/1998/Math/MathML" display="inline"> <t:msub> <t:mi>m</t:mi> <t:mi>χ</t:mi> </t:msub> </t:math> , though at the cost of tension with cosmological bounds. If the NANOGrav fits are viewed as constraints, given their comparatively lower Bayes factors, they yield bounds that are significantly stronger than those imposed by the CMB and other cosmological data.